Swift Cycle 22 Results
The lists below contain the proposals recommended by the Cycle 22 Peer Review panel. Note that in addition to the accepted programs below, ToO requests for exceptional transients will continue to be possible through the Swift ToO web site, even for ToOs not accepted into the GI Program. The decision on whether or not to observe a ToO of either category will be made by the Swift Principal Investigator.
PIs of Cycle 22 proposals for observation:
It is the responsibility of the Principal Investigator (PI) of an accepted ToO to alert the Swift Observatory Duty Scientist when trigger conditions for their accepted ToO have been met. This is done through the Swift ToO Request Form at https://www.swift.psu.edu/. It is highly recommended that ToO proposers register as Swift ToO users in advance at https://www.swift.psu.edu/. Registration is required in order to submit a ToO Request.
ToO proposals must have an astrophysical trigger. Once the trigger criteria have been met for an approved target, the PI should check if the target location is more than 47 degrees from the Sun and more than 23 degrees from the Moon before requesting Swift observations (http://heasarc.gsfc.nasa.gov/Tools/Viewing.html).
Accepted Cycle 22 ToO proposals may be triggered until March 31, 2027. -- PLEASE CONFIRM THIS BEFORE GOING LIVE
- To notify the Swift team that your trigger has occured, please use the Swift ToO web site and don't forget to use the proposal number for your proposal (below) when filling out the form.
Phase 2 budget proposals are due on 4:30 PM EDT on March 6, 2026. -- PLEASE CONFIRM THIS BEFORE GOING LIVE
Jump to:
Recommended Proposals
Prop PI Title
2225013 GRUPE UNDERSTANDING AGN VARIABILITY WITH RESPECT TO AGN PROPERTIES
2225035 KENNEA SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS IN CYCLE 22
2225037 KENNEA RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS IN CYCLE 22
2225040 KENNEA IDENTIFYING THE ELECTROMAGNETIC COUNTERPARTS TO COSMIC NEUTRINO SOURCES
2225050 HOLWERDA THE DUST ATTENUATION LAW IN OVERLAPPING GALAXY PAIRS
2225056 MARGUTTI XRT+NUSTAR PROMPT OBSERVATIONS OF STRONG SN SHOCK INTERACTION
2225061 MARCULEWICZ THE MISSING PIECE OF REVERBERATION MAPPING - LOW-MASS AGN NGC 4051
2225066 SAIKIA OBSERVING THE EARLY RISE OF X-RAY TRANSIENTS WITH SWIFT
2225067 HERNANDEZ SANTISTEBAN UNDERSTANDING AGN VARIABILITY WITH FAIRALL 9: A LEGACY SPECTROSCOPIC ECHO-MAPPING
EXPERIMENT WITH SWIFT AND HST
2225071 RAJGURU HUNTING EXTREME BLAZARS USING SWIFT-XRT
2225073 SALA MAGNETIC NOVAE: TWO NEW IP CANDIDATES AMONG HISTORICAL NOVAE
2225074 BENOIT LOW-LATENCY ALERTS FROM GRAVITATIONAL WAVE SIGNALS FOR SWIFT FOLLOW-UP
2225085 SRINIVASARAGAVAN FOLLOW UP X-RAY OBSERVATIONS OF X-RAY FLASH CANDIDATES DURING SWIFT CYCLE 22
2225086 VASYLYEV ULTRA-RAPID, HIGH-CADENCE UV PHOTOMETRY OF INFANT SUPERNOVAE
2225087 WILSON NUV PHOTOMETRY OF THE MOST LIKELY TARGETS FOR THE HABITABLE WORLDS OBSERVATORY
2225100 CHAKRABORTY UNDERSTANDING THE DIVERSITY OF LATE-TIME BEHAVIOR IN TIDAL DISRUPTION EVENTS
2225105 MASTERSON A LATE-TIME X-RAY VIEW OF MID-INFRARED-SELECTED TDE CANDIDATES
2225121 BORGHESE SWIFT MONITORING OF MAGNETAR OUTBURSTS
2225124 EVANS FOLLOW UP OF NEW X-RAY TRANSIENTS DETECTED BY SWIFT
2225125 DEGENAAR TOWARDS TWO DECADES OF SWIFT MONITORING OF THE GALACTIC CENTER
2225128 LAWTHER CAPTURING THE CONTINUED EVOLUTION OF AN EXTREME AGN
2225129 DEGENAAR THE NATURE AND ACCRETION FLOW PROPERTIES OF SUB-LUMINOUS X-RAY BINARIES
2225131 WOODWARD WAITING FOR GODOT - THE SWIFT T CORONAE BOREALIS REVEAL
2225136 CHAKRABORTY MONITORING THE EXTREME QUASI-PERIODIC ERUPTIONS IN ZTF19ACNSKYY
2225139 LINCETTO SWIFT FOLLOW UP OF KM3NET HIGH-ENERGY NEUTRINO EVENTS
2225144 NUNEZ CONTINUING THE X-RAY CENSUS OF GROUP-X, A NEW LABORATORY FOR INVESTIGATING THE
ACTIVITY-ROTATION RELATION
2225160 MARCOTULLI UNVEILING THE NATURE OF NEWLY DETECTED MEV GALACTIC SOURCES
2225162 KAPLAN SEARCHING FOR X-RAY EMISSION FROM NEW MAGNETIC TRANSIENTS DISCOVERED BY ASKAP/VAST
2225165 VIELIUTE EXTENDING SCALING RELATIONS OF THE AGN ACCRETION FLOW INTO THE LOW-MASS REGIME
2225166 SAIKIA A SWIFT LEGACY SURVEY OF XRBS IN OUTBURST: TRACKING ACCRETION IN ACTION
2225171 BODEWITS SWIFT/UVOT AND THE WATER CYCLE OF OORT CLOUD COMETS
2225173 BUSON BREAKING THE DEGENERACY WITH THE NEIL GEHRELS SWIFT OBSERVATORY AND NUSTAR
2225175 DELAUNAY DETECTING WITH SWIFT THE AFTERGLOW OF GRBS LOCALIZED BY THE NITRATES PIPELINE
2225180 MASTERSON THE QPO-CORONA CONNECTION IN THE ENIGMATIC AGN 1ES 1927+654
2225181 MILLER REVERBERATION MAPPING OF CHANGING-LOOK ACTIVE GALACTIC NUCLEUS NGC5273
2225186 ARCODIA USING XRT TIMING DATA TO ESTIMATE THE BH MASS IN ERO-QPE5
2225188 ARCODIA PROBING THE X-RAY VARIABILITY OF LOW-MASS POST-STARBURST GALAXIES WITH SWIFT-XRT
2225190 DELAUNAY INCREASING THE RATE OF WELL-LOCALIZED TRANSIENTS WITH BAT-GUANO
2225194 LIN TWO UNIQUE SOURCES IN A ROW: ESO 243-49 HLX-1 AND A NEWBORN HARD TIDAL DISRUPTION EVENT
2225201 QUIMBY UNLOCKING HIGH-REDSHIFT SUPERLUMINOUS SUPERNOVAE
2225205 SOKOLOSKI PRE-ERUPTION MONITORING OF T CRB
2225208 ANUMARLAPUDI ON THE NATURE OF EXTRAGALACTIC RADIO TRANSIENTS DISCOVERED BY ASKAP/VAST -- EXTREME
NUCLEAR VARIABILITY?
2225216 STEIN HIGH-REDSHIFT TDES FROM RUBIN TO ROMAN
2225238 FOLEY REDUCING TYPE IA SUPERNOVA DISTANCE BIASES BY SEPARATING REDDENING AND INTRINSIC COLOR
2225241 WALTON A TALE OF TWO PHASES? CONTINUED MONITORING OF NGC2283 ULX1
2225243 TROJA A SWIFT LOOK AT SUPERNOVA SHOCK BREAK-OUTS
2225244 DESAI REDRAWING THE HR DIAGRAM FOR MAGNETIC WHITE DWARFS
2225249 LUNDY ENERGETIC EXTREMA IN 4C+42.22: CHARACTERIZING THE MOST EXTREME HIGH SYNCHROTRON PEAKED
BL LACS WITH SWIFT-XRT
2225250 DURBAK RIMAS - RAPID INFRARED IMAGER-SPECTROMETER: A RECENTLY COMMISSIONED FACILITY FOR FAST
FOLLOW-UP OF HIGH-Z GRBS
2225252 CLARK COMBINING SWIFT & JWST TO BENCHMARK THE INTERPLAY BETWEEN RADIATION AND THE ISM, ACROSS
1 DEX IN METALLICITY
2225255 BROWN IMPROVING SMEARED SWIFT SUPERNOVAE WITH TEMPLATE OBSERVATIONS
Recommended Targets
Definition of Columns
- Proposal: Proposal number assigned by Swift mission
- PI: Principal Investigator's last name
- Target_Num: Target number as listed on the proposal form
- Target_Name: Target name as listed on proposal forms
- Time: Total observing time approved, in ksec
- ToO: "Y" if Target of Opportunity proposal, otherwise "N"
- RA: Right Ascension (equinox J2000) in degrees
- Dec: Declination (equinox J2000) in degrees
Prop | PI | Target_Num | Target_Name | Time [ ks ] | TOO | RA [deg] | Dec [deg] | 2225013 | GRUPE | 1 | RX J0022.5-3407 | 1 | N | 5.63917 | -34.12222 | 2225013 | GRUPE | 2 | ESO 242-G8 | 1 | N | 6.25083 | -45.49278 | 2225013 | GRUPE | 3 | TON S 180 | 1 | N | 14.33417 | -22.3825 | 2225013 | GRUPE | 4 | QSO 0056-36 | 1 | N | 14.65583 | -36.10139 | 2225013 | GRUPE | 5 | RX J0100-5113 | 1 | N | 15.11292 | -51.23167 | 2225013 | GRUPE | 6 | RX J0105.6-1416 | 1 | N | 16.41167 | -14.27056 | 2225013 | GRUPE | 7 | RX J0117-3826 | 1 | N | 19.3775 | -38.44167 | 2225013 | GRUPE | 8 | MS 0117-28 | 1 | N | 19.89875 | -28.35889 | 2225013 | GRUPE | 9 | RX J0128.1-1848 | 1 | N | 22.02792 | -18.80861 | 2225013 | GRUPE | 10 | IRAS F01267-217 | 1 | N | 22.29458 | -21.69917 | 2225013 | GRUPE | 11 | RX J0134.2-4258 | 1.4 | N | 23.57042 | -42.97417 | 2225013 | GRUPE | 12 | RX J0136.9-3510 | 1.25 | N | 24.22667 | -35.16444 | 2225013 | GRUPE | 13 | RX J0148.3-2758 | 1 | N | 27.09292 | -27.97389 | 2225013 | GRUPE | 14 | RX J0152.4-2319 | 1 | N | 28.11292 | -23.33167 | 2225013 | GRUPE | 15 | MKN 1044 | 1 | N | 37.52292 | -8.99806 | 2225013 | GRUPE | 16 | MKN 1048 | 1 | N | 38.6575 | -8.78778 | 2225013 | GRUPE | 17 | RX J0311.3-2046 | 1 | N | 47.82833 | -20.77194 | 2225013 | GRUPE | 18 | RX J0319.8-2627 | 1 | N | 49.95292 | -26.45333 | 2225013 | GRUPE | 19 | RX J0323.2-4931 | 1.4 | N | 50.81583 | -49.51972 | 2225013 | GRUPE | 20 | ESO 301-G13. | 1 | N | 51.26042 | -41.905 | 2225013 | GRUPE | 21 | VCV 0331-37. | 1 | N | 53.4175 | -37.11528 | 2225013 | GRUPE | 22 | RX J0349.1-4711 | 1.7 | N | 57.28208 | -47.18444 | 2225013 | GRUPE | 23 | FAIRALL 1116 | 1 | N | 57.92375 | -40.46667 | 2225013 | GRUPE | 24 | FAIRALL 1119 | 1 | N | 61.25708 | -37.1875 | 2225013 | GRUPE | 25 | RX J0412.7-4712 | 1 | N | 63.17292 | -47.21278 | 2225013 | GRUPE | 26 | 1H 0419-577 | 1 | N | 66.50292 | -57.20056 | 2225013 | GRUPE | 27 | FAIRALL 303 | 1 | N | 67.66667 | -53.61556 | 2225013 | GRUPE | 28 | RX J0435.2-4615 | 1 | N | 68.81 | -46.25917 | 2225013 | GRUPE | 29 | RX J0435.9-3636 | 1 | N | 68.97458 | -36.61139 | 2225013 | GRUPE | 30 | RX J0437.4-4711 | 1 | N | 69.3675 | -47.19167 | 2225013 | GRUPE | 31 | RX J0439.6-5311 | 1 | N | 69.91125 | -53.19194 | 2225013 | GRUPE | 32 | 1H 0439-272 | 1 | N | 70.34375 | -27.13889 | 2225013 | GRUPE | 33 | RX J0454.7-4813 | 1 | N | 73.67917 | -48.22222 | 2225013 | GRUPE | 34 | PKS 0558-504 | 1 | N | 89.9475 | -50.44778 | 2225013 | GRUPE | 35 | 1 ES 0614-584 | 1 | N | 93.95667 | -58.435 | 2225013 | GRUPE | 36 | RX J0859.0+4846 | 1 | N | 134.76208 | 48.76917 | 2225013 | GRUPE | 37 | RX J0902.5-0700 | 1.7 | N | 135.64 | -7.00111 | 2225013 | GRUPE | 38 | MKN 110 | 1 | N | 141.30417 | 52.28667 | 2225013 | GRUPE | 39 | PMN J0948+00222 | 1.4 | N | 147.2375 | 0.37361 | 2225013 | GRUPE | 40 | PG 0953+414 | 1 | N | 149.21833 | 41.25611 | 2225013 | GRUPE | 41 | RX J0435.2-4615 | 1 | N | 68.81 | -46.25917 | 2225013 | GRUPE | 42 | RX J1005.7+4332 | 1.25 | N | 151.42458 | 43.54472 | 2225013 | GRUPE | 43 | RX J1007.1+2203 | 1.4 | N | 151.7925 | 22.05056 | 2225013 | GRUPE | 44 | CBS 126 | 1 | N | 153.2625 | 35.85667 | 2225013 | GRUPE | 45 | RX J1017.3+2914 | 1 | N | 154.32625 | 29.24278 | 2225013 | GRUPE | 46 | HS 1019+37 | 1.25 | N | 154.75208 | 37.87806 | 2225013 | GRUPE | 47 | MKN 141 | 2 | N | 154.8025 | 63.9675 | 2225013 | GRUPE | 48 | MKN 142 | 1 | N | 156.38042 | 51.67639 | 2225013 | GRUPE | 49 | RX J1034.6+3938 | 1 | N | 158.66083 | 39.64111 | 2225013 | GRUPE | 50 | EXO 1055+60 | 1 | N | 164.62542 | 60.26694 | 2225013 | GRUPE | 51 | RX J1117.1+6522 | 1 | N | 169.29208 | 65.36861 | 2225013 | GRUPE | 52 | PG 1115+407 | 1 | N | 169.62667 | 40.43194 | 2225013 | GRUPE | 53 | TON 1388 | 1 | N | 169.78625 | 21.32167 | 2225013 | GRUPE | 54 | EXO 1128+69 | 1 | N | 172.77 | 68.86472 | 2225013 | GRUPE | 55 | 2B 1128+31 | 1 | N | 172.78958 | 31.235 | 2225013 | GRUPE | 56 | SBS 1136+579 | 1.25 | N | 174.70667 | 57.71222 | 2225013 | GRUPE | 57 | Z 1136+3412 | 1 | N | 174.80792 | 33.93083 | 2225013 | GRUPE | 58 | WAS 26 | 1 | N | 175.3175 | 21.93917 | 2225013 | GRUPE | 59 | CASG 855 | 2 | N | 176.12458 | 36.88583 | 2225013 | GRUPE | 60 | CSO 109 | 1 | N | 176.29292 | 30.78806 | 2225013 | GRUPE | 61 | MKN 1310 | 1 | N | 180.31 | -3.67806 | 2225013 | GRUPE | 62 | NGC 4051 | 1 | N | 180.78958 | 44.53056 | 2225013 | GRUPE | 63 | GQ COMAE | 1 | N | 181.17542 | 27.90333 | 2225013 | GRUPE | 64 | RX J1209.8+3217 | 2 | N | 182.43833 | 32.28389 | 2225013 | GRUPE | 65 | PG 1211+143 | 1 | N | 183.57375 | 14.05361 | 2225013 | GRUPE | 66 | MKN 766 | 1 | N | 184.61083 | 29.81278 | 2225013 | GRUPE | 67 | RX J1231.6+7044 | 1 | N | 187.9025 | 70.73722 | 2225013 | GRUPE | 68 | MKN 771 | 1 | N | 188.015. | 20.15833 | 2225013 | GRUPE | 69 | TON 83 | 1.4 | N | 188.42375 | 31.0175 | 2225013 | GRUPE | 70 | MCG+08-23-067 | 1.7 | N | 189.21333 | 45.65139 | 2225013 | GRUPE | 71 | NGC 4593 | 1 | N | 189.91417 | -5.34417 | 2225013 | GRUPE | 72 | IRAS F12397+3333 | 1 | N | 190.54417 | 33.28417 | 2225013 | GRUPE | 73 | PG 1244+026 | 1 | N | 191.64667 | 2.36917 | 2225013 | GRUPE | 74 | RX J1304.2+0205 | 2 | N | 196.07083 | 2.09361 | 2225013 | GRUPE | 75 | PG 1307+085 | 2 | N | 197.44583 | 8.33 | 2225013 | GRUPE | 76 | RX J1312.9+2628 | 2 | N | 198.24792 | 26.47417 | 2225013 | GRUPE | 77 | RX J1314.3+3429 | 2 | N | 198.59458 | 34.49417 | 2225013 | GRUPE | 78 | RX J1319.9+5235 | 1 | N | 199.98792 | 52.5925 | 2225013 | GRUPE | 79 | PG 1322+659 | 1.4 | N | 200.95625 | 65.69667 | 2225013 | GRUPE | 80 | IRAS 13349+2438 | 1 | N | 204.32792 | 24.38417 | 2225013 | GRUPE | 81 | TON 730 | 1 | N | 205.98625 | 25.64667 | 2225013 | GRUPE | 82 | 2E 13 46+2637 | 2 | N | 207.14292 | 26.36861 | 2225013 | GRUPE | 83 | RX J1355.2+5612 | 1 | N | 208.81917 | 56.2125 | 2225013 | GRUPE | 84 | PG 1402+261 | 1 | N | 211.3175 | 25.92611 | 2225013 | GRUPE | 85 | RX J1413.6+7029 | 1 | N | 213.40292 | 70.49722 | 2225013 | GRUPE | 86 | QSO 1421-0013 | 1 | N | 216.01583 | -0.44944 | 2225013 | GRUPE | 87 | MKN 813 | 1 | N | 216.85417 | 19.83139 | 2225013 | GRUPE | 88 | MKN 684 | 1 | N | 217.76708 | 28.28722 | 2225013 | GRUPE | 89 | MKN 478 | 1 | N | 220.53125 | 35.43972 | 2225013 | GRUPE | 90 | PG 1448+273 | 1 | N | 222.78667 | 27.1575 | 2225013 | GRUPE | 91 | MKN 841 | 1 | N | 226.005 | 10.43778 | 2225013 | GRUPE | 92 | SBS 1517+520 | 2 | N | 229.63667 | 51.91583 | 2225013 | GRUPE | 93 | SBS 1527+564 | 1 | N | 232.28125 | 56.26861 | 2225013 | GRUPE | 94 | MKN 493 | 2 | N | 239.79042 | 35.03 | 2225013 | GRUPE | 95 | MKN 876 | 1 | N | 243.48833 | 65.71972 | 2225013 | GRUPE | 96 | RX J1618.1+3619 | 1 | N | 244.53917 | 36.33278 | 2225013 | GRUPE | 97 | KUG 1618+40 | 2 | N | 244.96375 | 40.98. | 2225013 | GRUPE | 98 | PG 1626+554 | 1 | N | 246.98375 | 55.37556 | 2225013 | GRUPE | 99 | EXO 1627+4014 | 1.7 | N | 247.25542 | 40.13333 | 2225013 | GRUPE | 100 | RX J1646.4+3929 | 1 | N | 251.60833 | 39.4925 | 2225013 | GRUPE | 101 | RX J1702.5+3247 | 1 | N | 255.62958 | 32.78889 | 2225013 | GRUPE | 102 | PKS 2004-447. | 2 | N | 301.98 | -44.57889 | 2225013 | GRUPE | 103 | II ZW 136 | 1 | N | 323.11625 | 10.13889 | 2225013 | GRUPE | 104 | RX J2146.6-3051 | 1 | N | 326.65 | -30.86139 | 2225013 | GRUPE | 105 | RX J2154.8-4414 | 1 | N | 328.71333 | -44.235 | 2225013 | GRUPE | 106 | ESO 404-G029 | 1 | N | 331.9375 | -32.58361 | 2225013 | GRUPE | 107 | NGC 7214 | 1 | N | 332.27917 | -27.81 | 2225013 | GRUPE | 108 | RX J2213.0-1710 | 1 | N | 333.25125 | -17.17167 | 2225013 | GRUPE | 109 | RX J2216.8-4451 | 1 | N | 334.22167 | -44.86583 | 2225013 | GRUPE | 110 | RX J2217.9-5941 | 3 | N | 334.48583 | -59.69167 | 2225013 | GRUPE | 111 | PKS 2227-399 | 1 | N | 337.66792 | -39.71444 | 2225013 | GRUPE | 112 | RX J2241.9-4404 | 2 | N | 340.48167 | -44.08194 | 2225013 | GRUPE | 113 | RX J2242.6-3845 | 1.25 | N | 340.65708 | -38.75444 | 2225013 | GRUPE | 114 | RX J2245.2-4652 | 1.7 | N | 341.33458 | -46.87 | 2225013 | GRUPE | 115 | MS 2254-36 | 1 | N | 344.4125 | -36.93528 | 2225013 | GRUPE | 116 | RX J2258.7-2609 | 1 | N | 344.68917 | -26.15389 | 2225013 | GRUPE | 117 | RX J2301.6-5913 | 1 | N | 345.40083 | -59.22222 | 2225013 | GRUPE | 118 | RX J2301.8-5508 | 1.25 | N | 345.46667 | -55.14194 | 2225013 | GRUPE | 119 | RX J2303.9-5517 | 1 | N | 345.99167 | -55.28833 | 2225013 | GRUPE | 120 | RX J2304.6-3501 | 2 | N | 346.15542 | -35.02028 | 2225013 | GRUPE | 121 | RX J2312.5-3404 | 1.25 | N | 348.145 | -34.07222 | 2225013 | GRUPE | 122 | RX J2314.9+2243 | 2 | N | 348.73208 | 22.72278 | 2225013 | GRUPE | 123 | RX J2317.8-4422 | 2 | N | 349.45792 | -44.37444 | 2225013 | GRUPE | 124 | RX J2325.2-3236 | 1 | N | 351.29917 | -32.60972 | 2225013 | GRUPE | 125 | IRAS F23226-3843 | 2 | N | 351.35083 | -38.44694 | 2225013 | GRUPE | 126 | MS 23409-1511 | 1 | N | 355.86917 | -14.925 | 2225013 | GRUPE | 127 | RX J2349.4-3126 | 2 | N | 357.35042 | -31.43417 | 2225013 | GRUPE | 128 | AM 2354-304 | 1 | N | 359.36667 | -30.46111 | 2225035 | KENNEA | 1 | MAXI TRANSIENT #1 | 1 | Y | 0 | 0 | 2225035 | KENNEA | 2 | MAXI TRANSIENT #2 | 1 | Y | 0 | 0 | 2225035 | KENNEA | 3 | MAXI TRANSIENT #3 | 1 | Y | 0 | 0 | 2225035 | KENNEA | 4 | MAXI TRANSIENT #4 | 2 | Y | 0 | 0 | 2225035 | KENNEA | 5 | MAXI TRANSIENT #5 | 2 | Y | 0 | 0 | 2225035 | KENNEA | 6 | MAXI TRANSIENT #6 | 3.5 | Y | 0 | 0 | 2225037 | KENNEA | 1 | FRB #1 | 2 | Y | 0 | 0 | 2225037 | KENNEA | 2 | FRB #2 | 2 | Y | 0 | 0 | 2225037 | KENNEA | 3 | FRB #3 | 2 | Y | 0 | 0 | 2225037 | KENNEA | 4 | FRB #4 | 2 | Y | 0 | 0 | 2225037 | KENNEA | 5 | FRB #5 | 2 | Y | 0 | 0 | 2225037 | KENNEA | 6 | FRB #6 | 2 | Y | 0 | 0 | 2225037 | KENNEA | 7 | FRB #7 | 2 | Y | 0 | 0 | 2225037 | KENNEA | 8 | FRB #8 | 2 | Y | 0 | 0 | 2225037 | KENNEA | 9 | FRB #9 | 2 | Y | 0 | 0 | 2225037 | KENNEA | 10 | FRB #10 | 2 | Y | 0 | 0 | 2225040 | KENNEA | 1 | ICECUBE TRIGGER #1 | 9.5 | Y | 0 | 0 | 2225040 | KENNEA | 2 | ICECUBE TRIGGER #2 | 9.5 | Y | 0 | 0 | 2225040 | KENNEA | 3 | ICECUBE TRIGGER #3 | 18.5 | Y | 0 | 0 | 2225040 | KENNEA | 4 | KM3NET TRIGGER #1 | 3.5 | Y | 0 | 0 | 2225040 | KENNEA | 5 | KM3NET TRIGGER #2 | 9.5 | Y | 0 | 0 | 2225040 | KENNEA | 6 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2225040 | KENNEA | 7 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2225040 | KENNEA | 8 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2225040 | KENNEA | 9 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2225040 | KENNEA | 10 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2225050 | HOLWERDA | 1 | SDSS 2318+10 | 15 | N | 349.547 | 10.24611 | 2225050 | HOLWERDA | 2 | GAMA 3318 | 15 | N | 219.6945 | -1.5015 | 2225050 | HOLWERDA | 3 | UGC 9652 | 15 | N | 225.154 | 16.17228 | 2225050 | HOLWERDA | 4 | GAMA 4472 | 15 | N | 129.30679 | -1.64869 | 2225050 | HOLWERDA | 5 | GAMA 3378 | 15 | N | 130.64629 | 2.36689 | 2225050 | HOLWERDA | 6 | UGC 9125 | 15 | N | 213.784 | 45.59481 | 2225050 | HOLWERDA | 7 | SDSS 0856 | 15 | N | 134.153 | 51.49019 | 2225050 | HOLWERDA | 8 | UGC 4717 | 15 | N | 135.156 | 51.2075 | 2225050 | HOLWERDA | 9 | UGC 4070 | 15 | N | 118.36 | 50.22839 | 2225050 | HOLWERDA | 10 | SDSS 1021+17 | 15 | N | 155.455 | 17.92569 | 2225050 | HOLWERDA | 11 | GAMA 3219 | 15 | N | 220.9575 | -1.33581 | 2225050 | HOLWERDA | 12 | SDSS 0951 | 15 | N | 147.788 | 5.15567 | 2225050 | HOLWERDA | 13 | GAMA 1322 | 15 | N | 176.30771 | -2.305 | 2225050 | HOLWERDA | 14 | GAMA 2597 | 15 | N | 137.5795 | 2.18819 | 2225050 | HOLWERDA | 15 | SDSS 1336 | 15 | N | 204.177 | 62.06039 | 2225050 | HOLWERDA | 16 | SDSS 1149 | 15 | N | 177.299 | 56.75819 | 2225050 | HOLWERDA | 17 | SDSS 1411 | 15 | N | 212.789 | 54.94661 | 2225050 | HOLWERDA | 18 | UGC 10225 | 15 | N | 242.33642 | 8.76322 | 2225050 | HOLWERDA | 19 | UGC 4570 | 15 | N | 131.317 | 27.82369 | 2225050 | HOLWERDA | 20 | GAMA 2104 | 15 | N | 176.02162 | 1.36161 | 2225050 | HOLWERDA | 21 | SDSS 0914 | 15 | N | 138.70387 | 49.90197 | 2225050 | HOLWERDA | 22 | SDSS 1047+03 | 15 | N | 161.94642 | 3.33642 | 2225050 | HOLWERDA | 23 | GAMA 1326 | 15 | N | 176.36771 | -2.44839 | 2225050 | HOLWERDA | 24 | VV 191 | 15 | N | 207.09317 | 25.68047 | 2225050 | HOLWERDA | 25 | GAMA 4343 | 15 | N | 140.99042 | -1.43739 | 2225050 | HOLWERDA | 26 | GAMA 1009 | 15 | N | 185.38479 | -2.61169 | 2225050 | HOLWERDA | 27 | KUG 1600+12 | 15 | N | 240.66583 | 12.16886 | 2225050 | HOLWERDA | 28 | SDSS 2116+00 | 15 | N | 319.1825 | 0.17031 | 2225050 | HOLWERDA | 29 | GAMA 3178 | 15 | N | 222.67796 | -1.72642 | 2225050 | HOLWERDA | 30 | SDSS 0849+57 | 15 | N | 132.437 | 57.15642 | 2225056 | MARGUTTI | 1 | SNINTERACTING | 45 | Y | 0 | 0 | 2225061 | MARCULEWICZ | 1 | NGC 4051 | 156 | N | 180.79004 | 44.53131 | 2225066 | SAIKIA | 1 | TRANSIENT 1 | 20 | Y | 0 | 0 | 2225066 | SAIKIA | 2 | TRANSIENT 2 | 20 | Y | 0 | 0 | 2225067 | HERNANDEZ SANTISTEBAN | 1 | FAIRALL 9 | 182 | N | 20.94067 | -58.80578 | 2225071 | RAJGURU | 1 | 4FGL J1736.6+0628 | 16 | N | 264.11904 | 6.52986 | 2225071 | RAJGURU | 2 | 4FGL J2114.8+2831 | 6 | N | 318.743 | 28.54922 | 2225071 | RAJGURU | 3 | 4FGL J0743.0-5622 | 4 | N | 115.83529 | -56.32583 | 2225071 | RAJGURU | 4 | 4FGL J1747.4+2330 | 4 | N | 266.95858 | 23.41075 | 2225073 | SALA | 1 | RR CHA | 20 | N | 201.5995 | -82.32872 | 2225073 | SALA | 2 | AT CNC | 20 | N | 127.15387 | 25.33417 | 2225085 | SRINIVASARAGAVAN | 1 | XRF CANDIDATE 1 | 7.5 | Y | 0 | 0 | 2225085 | SRINIVASARAGAVAN | 2 | XRF CANDIDATE 2 | 7.5 | Y | 0 | 0 | 2225085 | SRINIVASARAGAVAN | 3 | XRF CANDIDATE 3 | 7.5 | Y | 0 | 0 | 2225085 | SRINIVASARAGAVAN | 4 | XRF CANDIDATE 4 | 7.5 | Y | 0 | 0 | 2225085 | SRINIVASARAGAVAN | 5 | XRF CANDIDATE 5 | 7.5 | Y | 0 | 0 | 2225085 | SRINIVASARAGAVAN | 6 | XRF CANDIDATE 6 | 7.5 | Y | 0 | 0 | 2225085 | SRINIVASARAGAVAN | 7 | XRF CANDIDATE 7 | 7.5 | Y | 0 | 0 | 2225086 | VASYLYEV | 1 | SN1 | 36 | Y | 0 | 0 | 2225086 | VASYLYEV | 2 | SN2 | 36 | Y | 0 | 0 | 2225086 | VASYLYEV | 3 | SN3 | 36 | Y | 0 | 0 | 2225086 | VASYLYEV | 4 | SN4 | 36 | Y | 0 | 0 | 2225086 | VASYLYEV | 5 | SN5 | 36 | Y | 0 | 0 | 2225087 | WILSON | 1 | TIC_238432056 | 1 | N | 1.65325 | 29.0215 | 2225087 | WILSON | 2 | TIC_434210589 | 1 | N | 9.84088 | 21.25047 | 2225087 | WILSON | 3 | TIC_80431620 | 1 | N | 11.43996 | -47.55197 | 2225087 | WILSON | 4 | TIC_257393898 | 1 | N | 12.09575 | 5.28061 | 2225087 | WILSON | 5 | TIC_231005052 | 1 | N | 24.94817 | -56.19644 | 2225087 | WILSON | 6 | TIC_231005905 | 1 | N | 24.94921 | -56.19331 | 2225087 | WILSON | 7 | TIC_373694425 | 1 | N | 26.93679 | 63.8525 | 2225087 | WILSON | 8 | TIC_72748794 | 1 | N | 34.74375 | -25.94569 | 2225087 | WILSON | 9 | TIC_30016911 | 1 | N | 43.13388 | -12.76972 | 2225087 | WILSON | 10 | TIC_118572803 | 1 | N | 53.23267 | -9.45825 | 2225087 | WILSON | 11 | TIC_311063391 | 1 | N | 85.33475 | 53.48106 | 2225087 | WILSON | 12 | TIC_282210766 | 1 | N | 103.07521 | -5.17372 | 2225087 | WILSON | 13 | TIC_393844873 | 1 | N | 128.21458 | -31.50086 | 2225087 | WILSON | 14 | TIC_181273463 | 1 | N | 130.82512 | -38.88239 | 2225087 | WILSON | 15 | TIC_8915802 | 1 | N | 143.91458 | 35.81014 | 2225087 | WILSON | 16 | TIC_371520835 | 1 | N | 152.84225 | 49.45425 | 2225087 | WILSON | 17 | TIC_57611256 | 1 | N | 173.62287 | -32.83133 | 2225087 | WILSON | 18 | TIC_101641846 | 1 | N | 175.26258 | 34.20164 | 2225087 | WILSON | 19 | TIC_309599261 | 1 | N | 178.24488 | 37.71869 | 2225087 | WILSON | 20 | TIC_373765355 | 1 | N | 199.21271 | 17.01717 | 2225087 | WILSON | 21 | TIC_202380743 | 1 | N | 209.38358 | 61.49286 | 2225087 | WILSON | 22 | TIC_287157634 | 1 | N | 224.36667 | -21.41547 | 2225087 | WILSON | 23 | TIC_179348425 | 1 | N | 236.87125 | -37.91631 | 2225087 | WILSON | 24 | TIC_58092025 | 1 | N | 249.08938 | -2.32458 | 2225087 | WILSON | 25 | TIC_1277142191 | 1 | N | 258.83658 | -26.60169 | 2225087 | WILSON | 26 | TIC_1277142190 | 1 | N | 258.83742 | -26.60283 | 2225087 | WILSON | 27 | TIC_79841001 | 1 | N | 259.05567 | -26.54614 | 2225087 | WILSON | 28 | TIC_217157387 | 1 | N | 259.766 | -46.63622 | 2225087 | WILSON | 29 | TIC_219880402 | 1 | N | 261.25042 | 67.30669 | 2225087 | WILSON | 30 | TIC_75946144 | 1 | N | 272.40592 | 38.45778 | 2225087 | WILSON | 31 | TIC_389198736 | 1 | N | 302.79975 | -36.10122 | 2225087 | WILSON | 32 | TIC_165602000 | 1 | N | 316.72475 | 38.74942 | 2225087 | WILSON | 33 | TIC_165602023 | 1 | N | 316.73025 | 38.74206 | 2225087 | WILSON | 34 | TIC_231698181 | 1 | N | 330.84021 | -56.78597 | 2225087 | WILSON | 35 | TIC_206686962 | 1 | N | 344.10021 | -31.56556 | 2225087 | WILSON | 36 | TIC_283722336 | 1 | N | 348.32071 | 57.16836 | 2225100 | CHAKRABORTY | 1 | 2XMMI J184725.1-6317 | 2 | N | 281.85417 | -63.29028 | 2225100 | CHAKRABORTY | 2 | 3XMM J150052.0+01545 | 2 | N | 225.21667 | 1.91494 | 2225100 | CHAKRABORTY | 3 | 3XMM J152130.7+07491 | 2 | N | 230.37917 | 7.82125 | 2225100 | CHAKRABORTY | 4 | 3XMM J215022.4-05510 | 2 | N | 327.59167 | -5.85222 | 2225100 | CHAKRABORTY | 5 | ASASSN-14AE | 2 | N | 167.16667 | 34.09783 | 2225100 | CHAKRABORTY | 6 | ASASSN-14LI | 2 | N | 192.0625 | 17.774 | 2225100 | CHAKRABORTY | 7 | ASASSN-15LH | 2 | N | 330.5625 | -61.65972 | 2225100 | CHAKRABORTY | 8 | ASASSN-15OI | 2 | N | 309.7875 | -30.75556 | 2225100 | CHAKRABORTY | 9 | ASASSN-20IL | 2 | N | 75.79583 | -22.81444 | 2225100 | CHAKRABORTY | 10 | AT2016EZH | 2 | N | 29.52083 | 0.87278 | 2225100 | CHAKRABORTY | 11 | AT2017EQX | 2 | N | 336.7 | 17.14778 | 2225100 | CHAKRABORTY | 12 | AT2018BSI | 2 | N | 123.86092 | 45.59219 | 2225100 | CHAKRABORTY | 13 | AT2018CQH | 2 | N | 38.44554 | -1.02456 | 2225100 | CHAKRABORTY | 14 | AT2018DYB | 2 | N | 242.74487 | -60.92311 | 2225100 | CHAKRABORTY | 15 | AT2018FYK | 2 | N | 342.56658 | -44.86481 | 2225100 | CHAKRABORTY | 16 | AT2018HCO | 2 | N | 16.89012 | 23.47617 | 2225100 | CHAKRABORTY | 17 | AT2018HYZ | 2 | N | 151.712. | 1.69278 | 2225100 | CHAKRABORTY | 18 | AT2018IIH | 2 | N | 262.01629 | 30.69206 | 2225100 | CHAKRABORTY | 19 | AT2018JBV | 2 | N | 197.68983 | 8.56786 | 2225100 | CHAKRABORTY | 20 | AT2018LNA | 2 | N | 105.82771 | 23.02908 | 2225100 | CHAKRABORTY | 21 | AT2018LNI | 2 | N | 62.40688 | 73.89492 | 2225100 | CHAKRABORTY | 22 | AT2018ZR | 2 | N | 119.22729 | 34.26211 | 2225100 | CHAKRABORTY | 23 | AT2019AHK | 2 | N | 105.04812 | -66.04003 | 2225100 | CHAKRABORTY | 24 | AT2019AZH | 2 | N | 123.32058 | 22.64831 | 2225100 | CHAKRABORTY | 25 | AT2019BAF | 2 | N | 268.00063 | 65.62667 | 2225100 | CHAKRABORTY | 26 | AT2019BHF | 2 | N | 227.3165 | 16.23956 | 2225100 | CHAKRABORTY | 27 | AT2019CHO | 2 | N | 193.78837 | 49.51942 | 2225100 | CHAKRABORTY | 28 | AT2019CMW | 2 | N | 282.16446 | 51.01353 | 2225100 | CHAKRABORTY | 29 | AT2019DSG | 2 | N | 314.26229 | 14.2045 | 2225100 | CHAKRABORTY | 30 | AT2019EHZ | 2 | N | 212.4245 | 55.49111 | 2225100 | CHAKRABORTY | 31 | AT2019EVE | 2 | N | 172.20687 | 15.67286 | 2225100 | CHAKRABORTY | 32 | AT2019LWU | 2 | N | 347.80129 | -1.00297 | 2225100 | CHAKRABORTY | 33 | AT2019MEG | 2 | N | 281.31742 | 44.43867 | 2225100 | CHAKRABORTY | 34 | AT2019MHA | 2 | N | 244.11583 | 56.43231 | 2225100 | CHAKRABORTY | 35 | AT2019QIZ | 2 | N | 71.65783 | -10.22631 | 2225100 | CHAKRABORTY | 36 | AT2019TEQ | 2 | N | 284.77292 | 47.51825 | 2225100 | CHAKRABORTY | 37 | AT2019VCB | 2 | N | 189.73479 | 33.16586 | 2225100 | CHAKRABORTY | 38 | AT2020ABRI | 2 | N | 202.322 | 19.67092 | 2225100 | CHAKRABORTY | 39 | AT2020ACKA | 2 | N | 238.75808 | 16.30453 | 2225100 | CHAKRABORTY | 40 | AT2020ADGM | 2 | N | 63.26021 | -53.07269 | 2225100 | CHAKRABORTY | 41 | AT2020DDV | 2 | N | 149.63904 | 46.91119 | 2225100 | CHAKRABORTY | 42 | AT2020KSF | 2 | N | 323.86358 | -18.27653 | 2225100 | CHAKRABORTY | 43 | AT2020MBQ | 2 | N | 235.06367 | 25.00136 | 2225100 | CHAKRABORTY | 44 | AT2020MOT | 2 | N | 7.80625 | 85.00881 | 2225100 | CHAKRABORTY | 45 | AT2020NEH | 2 | N | 230.33371 | 14.06958 | 2225100 | CHAKRABORTY | 46 | AT2020NOV | 2 | N | 254.55408 | 2.1175 | 2225100 | CHAKRABORTY | 47 | AT2020OCN | 2 | N | 208.47442 | 53.99733 | 2225100 | CHAKRABORTY | 48 | AT2020OPY | 2 | N | 239.10721 | 23.37253 | 2225100 | CHAKRABORTY | 49 | AT2020PJ | 2 | N | 232.89571 | 33.09489 | 2225100 | CHAKRABORTY | 50 | AT2020QHS | 2 | N | 34.47487 | -9.61414 | 2225100 | CHAKRABORTY | 51 | AT2020RIZ | 2 | N | 32.62817 | 9.07408 | 2225100 | CHAKRABORTY | 52 | AT2020VDQ | 2 | N | 152.22267 | 42.71672 | 2225100 | CHAKRABORTY | 53 | AT2020VWL | 2 | N | 232.6575 | 26.98242 | 2225100 | CHAKRABORTY | 54 | AT2020WEY | 2 | N | 136.35779 | 61.80256 | 2225100 | CHAKRABORTY | 55 | AT2020YSG | 2 | N | 171.35842 | 27.44061 | 2225100 | CHAKRABORTY | 56 | AT2020YUE | 2 | N | 165.00137 | 21.11272 | 2225100 | CHAKRABORTY | 57 | AT2020ZSO | 2 | N | 335.57129 | -7.26636 | 2225100 | CHAKRABORTY | 58 | AT2021ACK | 2 | N | 208.29162 | 9.74036 | 2225100 | CHAKRABORTY | 59 | AT2021AXU | 2 | N | 176.6515 | 30.08542 | 2225100 | CHAKRABORTY | 60 | AT2021BLZ | 2 | N | 68.13021 | -32.43067 | 2225100 | CHAKRABORTY | 61 | AT2021CRK | 2 | N | 176.27896 | 18.54036 | 2225100 | CHAKRABORTY | 62 | AT2021EHB | 2 | N | 46.94925 | 40.31133 | 2225100 | CHAKRABORTY | 63 | AT2021GJE | 2 | N | 252.53054 | 34.81883 | 2225100 | CHAKRABORTY | 64 | AT2021JJM | 2 | N | 219.87771 | -27.8585 | 2225100 | CHAKRABORTY | 65 | AT2021JSG | 2 | N | 167.15296 | 30.76128 | 2225100 | CHAKRABORTY | 66 | AT2021LO | 2 | N | 46.10979 | 4.74564 | 2225100 | CHAKRABORTY | 67 | AT2021MHG | 2 | N | 4.92871 | 29.31686 | 2225100 | CHAKRABORTY | 68 | AT2021NWA | 2 | N | 238.46371 | 55.58878 | 2225100 | CHAKRABORTY | 69 | AT2021QTH | 2 | N | 302.91221 | -21.16017 | 2225100 | CHAKRABORTY | 70 | AT2021QXV | 2 | N | 229.74708 | -3.19586 | 2225100 | CHAKRABORTY | 71 | AT2021SDU | 2 | N | 17.84958 | 50.57489 | 2225100 | CHAKRABORTY | 72 | AT2021UQV | 2 | N | 8.16617 | 22.54889 | 2225100 | CHAKRABORTY | 73 | AT2021UTQ | 2 | N | 229.62117 | 73.35872 | 2225100 | CHAKRABORTY | 74 | AT2021UVZ | 2 | N | 263.21046 | 33.03289 | 2225100 | CHAKRABORTY | 75 | AT2021YTE | 2 | N | 103.76971 | 12.63417 | 2225100 | CHAKRABORTY | 76 | AT2021YZV | 2 | N | 105.2775 | 40.82517 | 2225100 | CHAKRABORTY | 77 | AT2022ADM | 2 | N | 216.96429 | 28.17478 | 2225100 | CHAKRABORTY | 78 | AT2022AEE | 2 | N | 132.18008 | 80.88328 | 2225100 | CHAKRABORTY | 79 | AT2022ARB | 2 | N | 156.043 | -0.823 | 2225100 | CHAKRABORTY | 80 | AT2022BDW | 2 | N | 126.29308 | 18.58264 | 2225100 | CHAKRABORTY | 81 | AT2022CZY | 2 | N | 185.50471 | 16.99556 | 2225100 | CHAKRABORTY | 82 | AT2022DBL | 2 | N | 185.18779 | 49.55128 | 2225100 | CHAKRABORTY | 83 | AT2022DSB | 2 | N | 235.59058 | -22.67056 | 2225100 | CHAKRABORTY | 84 | AT2022DYT | 2 | N | 150.03329 | 26.46069 | 2225100 | CHAKRABORTY | 85 | AT2022EXR | 2 | N | 262.46042 | 25.84217 | 2225100 | CHAKRABORTY | 86 | AT2022FPX | 2 | N | 232.76542 | 53.40536 | 2225100 | CHAKRABORTY | 87 | AT2022GDW | 2 | N | 208.49258 | 50.04175 | 2225100 | CHAKRABORTY | 88 | AT2022GRI | 2 | N | 109.5865 | 33.99486 | 2225100 | CHAKRABORTY | 89 | AT2022HVP | 2 | N | 148.6885 | 55.44036 | 2225100 | CHAKRABORTY | 90 | AT2022IBQ | 2 | N | 267.64908 | 21.27497 | 2225100 | CHAKRABORTY | 91 | AT2022LRI | 2 | N | 35.03338 | -22.72089 | 2225100 | CHAKRABORTY | 92 | AT2022PNA | 2 | N | 25.48142 | -3.28961 | 2225100 | CHAKRABORTY | 93 | AT2022RZ | 2 | N | 234.49 | 56.27161 | 2225100 | CHAKRABORTY | 94 | AT2022UPJ | 2 | N | 5.98692 | -14.42319 | 2225100 | CHAKRABORTY | 95 | AT2022WTN | 2 | N | 350.84908 | 10.6855 | 2225100 | CHAKRABORTY | 96 | AT2023CLX | 2 | N | 175.03917 | 15.32736 | 2225100 | CHAKRABORTY | 97 | AT2023CVB | 2 | N | 288.607 | 41.66925 | 2225100 | CHAKRABORTY | 98 | AT2023LLI | 2 | N | 344.41446 | 40.54444 | 2225100 | CHAKRABORTY | 99 | AT2023MHS | 2 | N | 205.81529 | 19.25025 | 2225100 | CHAKRABORTY | 100 | ATLAS18MLW | 2 | N | 113.93683 | 66.62147 | 2225100 | CHAKRABORTY | 101 | CSS100217 | 2 | N | 157.30417 | 40.7055 | 2225100 | CHAKRABORTY | 102 | ERASST J0456-20 | 2 | N | 74.20958 | -20.63056 | 2225100 | CHAKRABORTY | 103 | ERASST J074426.3+291 | 2 | N | 116.10888 | 29.26872 | 2225100 | CHAKRABORTY | 104 | F01004-2237 | 2 | N | 15.70833 | -22.36583 | 2225100 | CHAKRABORTY | 105 | GSN 069 | 2 | N | 19.78333 | -34.19167 | 2225100 | CHAKRABORTY | 106 | IPTF16AXA | 2 | N | 255.89167 | 30.5935 | 2225100 | CHAKRABORTY | 107 | IPTF16FNL | 2 | N | 7.4875 | 32.89367 | 2225100 | CHAKRABORTY | 108 | J155223 | 2 | N | 238.09583 | 32.58197 | 2225100 | CHAKRABORTY | 109 | NGC 3599 | 2 | N | 168.8625 | 18.11036 | 2225100 | CHAKRABORTY | 110 | NGC 5905 | 2 | N | 228.84583 | 55.51711 | 2225100 | CHAKRABORTY | 111 | OGLE16AAA | 2 | N | 16.8375 | -64.2725 | 2225100 | CHAKRABORTY | 112 | OGLE17AAJ | 2 | N | 29.10417 | -71.07111 | 2225100 | CHAKRABORTY | 113 | PGC 1127938 | 2 | N | 19.68333 | -1.15194 | 2225100 | CHAKRABORTY | 114 | PGC 1185375 | 2 | N | 225.95833 | 1.12686 | 2225100 | CHAKRABORTY | 115 | PGC 1190358 | 2 | N | 226.37083 | 1.29256 | 2225100 | CHAKRABORTY | 116 | PGC 133344 | 2 | N | 325.73333 | -30.13278 | 2225100 | CHAKRABORTY | 117 | PGC 170392 | 2 | N | 336.69167 | -15.02306 | 2225100 | CHAKRABORTY | 118 | PS1-10ADI | 2 | N | 310.6875 | 15.50892 | 2225100 | CHAKRABORTY | 119 | PS1-10JH | 2 | N | 242.36667 | 53.67333 | 2225100 | CHAKRABORTY | 120 | PS1-11AF | 2 | N | 149.3625 | 3.23358 | 2225100 | CHAKRABORTY | 121 | PS1-13JW | 2 | N | 131.225 | 42.96244 | 2225100 | CHAKRABORTY | 122 | PTF09AXC | 2 | N | 223.30417 | 22.24231 | 2225100 | CHAKRABORTY | 123 | PTF09DJL | 2 | N | 248.48333 | 30.23794 | 2225100 | CHAKRABORTY | 124 | PTF09GE | 2 | N | 224.2625 | 49.61139 | 2225100 | CHAKRABORTY | 125 | PTF10IYA | 2 | N | 219.67083 | 37.65931 | 2225100 | CHAKRABORTY | 126 | PTF10NUJ | 2 | N | 246.60417 | 54.70594 | 2225100 | CHAKRABORTY | 127 | RX J1242-11A | 2 | N | 190.65417 | -11.32639 | 2225100 | CHAKRABORTY | 128 | RX J133157.6-324319. | 2 | N | 202.99058 | -32.72219 | 2225100 | CHAKRABORTY | 129 | RX J1420+53 | 2 | N | 215.1 | 53.56992 | 2225100 | CHAKRABORTY | 130 | SDSS J134244.4+05305 | 2 | N | 205.68508 | 5.51558 | 2225100 | CHAKRABORTY | 131 | SDSS J143359.16+4006 | 2 | N | 218.4965 | 40.11 | 2225100 | CHAKRABORTY | 132 | SDSS J143359.16+4006 | 2 | N | 218.4965 | 40.11 | 2225100 | CHAKRABORTY | 133 | SDSS J152717.95+1645 | 2 | N | 231.82479 | 16.75081 | 2225100 | CHAKRABORTY | 134 | SDSSJ0159 | 2 | N | 29.99167 | 0.55292 | 2225100 | CHAKRABORTY | 135 | SDSSJ0952 | 2 | N | 148.04167 | 21.72033 | 2225100 | CHAKRABORTY | 136 | SDSSJ1201+30 | 2 | N | 180.4 | 30.05153 | 2225100 | CHAKRABORTY | 137 | SDSSJ1311 | 2 | N | 197.84167 | -1.39611 | 2225100 | CHAKRABORTY | 138 | SDSSJ1323 | 2 | N | 200.925 | 48.45036 | 2225100 | CHAKRABORTY | 139 | SDSSJ1342 | 2 | N | 205.68333 | 5.51558 | 2225100 | CHAKRABORTY | 140 | SDSSJ1350 | 2 | N | 207.50833 | 29.26936 | 2225100 | CHAKRABORTY | 141 | SN2017BCC | 2 | N | 172.97083 | 29.99578 | 2225100 | CHAKRABORTY | 142 | SRGE J013204.6+12223 | 2 | N | 23.01867 | 12.37656 | 2225100 | CHAKRABORTY | 143 | SRGE J021939.9+36181 | 2 | N | 34.91625 | 36.30506 | 2225100 | CHAKRABORTY | 144 | SRGE J071310.6+72562 | 2 | N | 108.29383 | 72.94075 | 2225100 | CHAKRABORTY | 145 | SRGE J091747.6+52482 | 2 | N | 139.4475 | 52.80564 | 2225100 | CHAKRABORTY | 146 | SRGE J095928.6+64302 | 2 | N | 149.86867 | 64.50606 | 2225100 | CHAKRABORTY | 147 | SRGE J133053.3+73482 | 2 | N | 202.72092 | 73.80675 | 2225100 | CHAKRABORTY | 148 | SRGE J135514.8+31160 | 2 | N | 208.81258 | 31.26811 | 2225100 | CHAKRABORTY | 149 | SRGE J144738.4+67182 | 2 | N | 221.91279 | 67.30508 | 2225100 | CHAKRABORTY | 150 | SRGE J153503.4+45505 | 2 | N | 233.76317 | 45.84861 | 2225100 | CHAKRABORTY | 151 | SRGE J161001.2+33012 | 2 | N | 242.50592 | 33.02242 | 2225100 | CHAKRABORTY | 152 | SRGE J163030.2+47012 | 2 | N | 247.62604 | 47.02372 | 2225100 | CHAKRABORTY | 153 | SRGE J163831.7+53402 | 2 | N | 249.63342 | 53.67294 | 2225100 | CHAKRABORTY | 154 | SRGE J171423.6+08523 | 2 | N | 258.59838 | 8.87692 | 2225100 | CHAKRABORTY | 155 | SWIFT J1112-82 | 2 | N | 167.95 | -82.64583 | 2225100 | CHAKRABORTY | 156 | SWIFT J1644+57 | 2 | N | 251.20417 | 57.58083 | 2225100 | CHAKRABORTY | 157 | SWIFT J2058+05 | 2 | N | 314.58333 | 5.22583 | 2225100 | CHAKRABORTY | 158 | T1 (2MASX J00414632- | 2 | N | 10.443 | -28.46178 | 2225100 | CHAKRABORTY | 159 | T2 (GAMA 91637) | 2 | N | 212.87583 | 0.47211 | 2225100 | CHAKRABORTY | 160 | T3 (XXL-AAOMEGA J234 | 2 | N | 355.73308 | -54.49961 | 2225100 | CHAKRABORTY | 161 | T4 (SDSS J152717.95+ | 2 | N | 231.82479 | 16.75086 | 2225100 | CHAKRABORTY | 162 | TDE2 | 2 | N | 350.95417 | -1.13611 | 2225100 | CHAKRABORTY | 163 | UGC 01791 | 2 | N | 34.975 | 28.24794 | 2225100 | CHAKRABORTY | 164 | UGC 03317 | 2 | N | 83.40833 | 73.72397 | 2225100 | CHAKRABORTY | 165 | WINGS J134849.88+263 | 2 | N | 207.20833 | 26.59931 | 2225100 | CHAKRABORTY | 166 | XMMSL1 J020303.1-074 | 2 | N | 30.76292 | -7.69833 | 2225100 | CHAKRABORTY | 167 | XMMSL1 J024916.6-041 | 2 | N | 42.31917 | -4.21222 | 2225100 | CHAKRABORTY | 168 | XMMSL1 J061927.1-655 | 2 | N | 94.86292 | -65.88639 | 2225100 | CHAKRABORTY | 169 | XMMSL1 J063045.9-603 | 2 | N | 115.03333 | 85.6575 | 2225100 | CHAKRABORTY | 170 | XMMSL1 J074008.2-853 | 2 | N | 115.03417 | -85.6575 | 2225100 | CHAKRABORTY | 171 | XMMSL1 J093922.5+370 | 2 | N | 144.84375 | 37.1625 | 2225100 | CHAKRABORTY | 172 | XMMSL1 J111527.3+180 | 2 | N | 168.86375 | 18.11056 | 2225100 | CHAKRABORTY | 173 | XMMSL1 J131952.3+225 | 2 | N | 97.69167 | -60.51944 | 2225100 | CHAKRABORTY | 174 | XMMSL1 J132342.3+482 | 2 | N | 200.92625 | 48.45028 | 2225100 | CHAKRABORTY | 175 | XMMSL2 J140446.9-251 | 2 | N | 211.19583 | -25.19306 | 2225100 | CHAKRABORTY | 176 | XMMSL2 J144605.0+685 | 2 | N | 221.52083 | 68.95861 | 2225100 | CHAKRABORTY | 177 | ERASSU_J011430.8-593 | 2 | N | 18.62829 | -59.61486 | 2225100 | CHAKRABORTY | 178 | 1ERASS_J014133.4-443 | 2 | N | 25.38987 | -44.57067 | 2225100 | CHAKRABORTY | 179 | 1ERASS_J024049.7-595 | 2 | N | 40.20571 | -59.90889 | 2225100 | CHAKRABORTY | 180 | 1ERASS_J031857.2-205 | 2 | N | 49.73929 | -20.91422 | 2225100 | CHAKRABORTY | 181 | 1ERASS_J034004.8-380 | 2 | N | 55.02058 | -38.0005 | 2225100 | CHAKRABORTY | 182 | 1ERASS_J034117.4-455 | 2 | N | 55.32154 | -45.95522 | 2225100 | CHAKRABORTY | 183 | 1ERASS_J043959.6-651 | 2 | N | 69.99796 | -65.23425 | 2225100 | CHAKRABORTY | 184 | ERASSU_J060829.4-435 | 2 | N | 92.1225 | -43.88881 | 2225100 | CHAKRABORTY | 185 | ERASSU_J061508.1-445 | 2 | N | 93.78363 | -44.98922 | 2225100 | CHAKRABORTY | 186 | ERASSU_J063413.3-713 | 2 | N | 98.55554 | -71.65219 | 2225100 | CHAKRABORTY | 187 | 1ERASS_J064449.4-603 | 2 | N | 101.20533 | -60.61756 | 2225100 | CHAKRABORTY | 188 | ERASSU_J070709.4-842 | 2 | N | 106.78929 | -84.34547 | 2225100 | CHAKRABORTY | 189 | ERASSU_J074426.3+291 | 2 | N | 116.10967 | 29.26822 | 2225100 | CHAKRABORTY | 190 | ERASSU_J082055.8+192 | 2 | N | 125.23254 | 19.42714 | 2225100 | CHAKRABORTY | 191 | 1ERASS_J082336.8+042 | 2 | N | 125.90329 | 4.38378 | 2225100 | CHAKRABORTY | 192 | 1ERASS_J084717.3-751 | 2 | N | 131.82708 | -75.18086 | 2225100 | CHAKRABORTY | 193 | 1ERASS_J091657.8+060 | 2 | N | 139.24079 | 6.16556 | 2225100 | CHAKRABORTY | 194 | 1ERASS_J110240.0-051 | 2 | N | 165.66692 | -5.30383 | 2225100 | CHAKRABORTY | 195 | 1ERASS_J130535.7+014 | 2 | N | 196.3995 | 1.7835 | 2225100 | CHAKRABORTY | 196 | ERASSU_J140158.1+081 | 2 | N | 210.49221 | 8.23397 | 2225100 | CHAKRABORTY | 197 | 1ERASS_J142140.3-295 | 2 | N | 215.41512 | -29.88922 | 2225100 | CHAKRABORTY | 198 | 1ERASS_J143623.9-174 | 2 | N | 219.09954 | -17.68478 | 2225100 | CHAKRABORTY | 199 | ERASSU_J145622.8-283 | 2 | N | 224.09512 | -28.64806 | 2225100 | CHAKRABORTY | 200 | ERASSU_J145954.5-260 | 2 | N | 224.97717 | -26.13958 | 2225100 | CHAKRABORTY | 201 | 1ERASS_J153406.2-090 | 2 | N | 233.52575 | -9.05906 | 2225100 | CHAKRABORTY | 202 | ERASSU_J164649.4-692 | 2 | N | 251.70579 | -69.4275 | 2225100 | CHAKRABORTY | 203 | 1ERASS_J173029.5-850 | 2 | N | 262.60796 | -85.08419 | 2225100 | CHAKRABORTY | 204 | 1ERASS_J190146.6-552 | 2 | N | 285.44437 | -55.36639 | 2225100 | CHAKRABORTY | 205 | 1ERASS_J192128.0-502 | 2 | N | 290.36771 | -50.46544 | 2225100 | CHAKRABORTY | 206 | 1ERASS_J210857.6-562 | 2 | N | 317.24354 | -56.47542 | 2225100 | CHAKRABORTY | 207 | ERASSU_J234403.1-352 | 2 | N | 356.01296 | -35.44456 | 2225105 | MASTERSON | 1 | WTP15ABUPKT | 2 | N | 242.77379 | 2.56675 | 2225105 | MASTERSON | 2 | WTP16AAVEGO | 2 | N | 161.50658 | -36.30236 | 2225105 | MASTERSON | 3 | WTP15ABZOOA | 2 | N | 254.36171 | 23.75783 | 2225105 | MASTERSON | 4 | WTP17AANKKJ | 2 | N | 178.52088 | -5.83333 | 2225105 | MASTERSON | 5 | WTP16AASRAL | 2 | N | 10.93592 | -33.944 | 2225105 | MASTERSON | 6 | WTP10ACPIKA | 2 | N | 80.44062 | -30.29619 | 2225105 | MASTERSON | 7 | WTP17AAKTGS | 2 | N | 13.94962 | -61.60772 | 2225105 | MASTERSON | 8 | WTP11AADIVN | 2 | N | 55.43542 | -53.70597 | 2225105 | MASTERSON | 9 | WTP10ACPIKA | 2 | N | 80.44062 | -30.29619 | 2225105 | MASTERSON | 10 | WTP17AALMPS | 2 | N | 15.835 | 14.03125 | 2225105 | MASTERSON | 11 | WTP17AAHYUS | 2 | N | 96.44021 | -4.36783 | 2225105 | MASTERSON | 12 | WTP14ADCCAD | 2 | N | 203.14129 | 44.39344 | 2225105 | MASTERSON | 13 | WTP17AAMOXE | 2 | N | 317.24237 | -56.47533 | 2225105 | MASTERSON | 14 | WTP14ADCADY | 2 | N | 9.78654 | -23.98792 | 2225105 | MASTERSON | 15 | WTP10ADERAJ | 2 | N | 310.32421 | -45.15436 | 2225105 | MASTERSON | 16 | WTP11AADGEF | 2 | N | 234.29712 | 58.23894 | 2225105 | MASTERSON | 17 | WTP17AANASC | 2 | N | 147.84437 | 22.12125 | 2225105 | MASTERSON | 18 | WTP17AAEAKZ | 2 | N | 157.58004 | -47.31086 | 2225105 | MASTERSON | 19 | WTP16AAPEIB | 2 | N | 210.58858 | 39.36969 | 2225105 | MASTERSON | 20 | WTP17AALMRA | 2 | N | 197.31808 | -44.77981 | 2225105 | MASTERSON | 21 | WTP14ADALRP | 2 | N | 125.126 | -5.08014 | 2225105 | MASTERSON | 22 | WTP17AALTJC | 2 | N | 219.26796 | -40.08967 | 2225105 | MASTERSON | 23 | WTP15ABYRAK | 2 | N | 215.7255 | 6.16489 | 2225105 | MASTERSON | 24 | WTP17AAJCJL | 2 | N | 36.72146 | 41.69031 | 2225105 | MASTERSON | 25 | WTP15ABXFYC | 2 | N | 314.33442 | 12.21256 | 2225105 | MASTERSON | 26 | WTP15ABXQUS | 2 | N | 168.90238 | 5.74717 | 2225105 | MASTERSON | 27 | WTP15ABWFGK | 2 | N | 136.91133 | 56.73281 | 2225105 | MASTERSON | 28 | WTP16AARLOY | 2 | N | 323.19696 | -60.29908 | 2225105 | MASTERSON | 29 | WTP18AAKFQB | 2 | N | 252.15825 | 1.47078 | 2225105 | MASTERSON | 30 | WTP15ACCELY | 2 | N | 174.13721 | -29.09067 | 2225105 | MASTERSON | 31 | WTP15ABVDFA | 2 | N | 89.79704 | -31.4425 | 2225105 | MASTERSON | 32 | WTP15ACBUUV | 2 | N | 154.67258 | -13.00189 | 2225105 | MASTERSON | 33 | WTP16AASVGC | 2 | N | 174.40692 | -43.32983 | 2225105 | MASTERSON | 34 | WTP14ADEQKA | 2 | N | 297.3535 | 63.50919 | 2225105 | MASTERSON | 35 | WTP16AAPTDI | 2 | N | 229.68646 | -21.94622 | 2225105 | MASTERSON | 36 | WTP10AATEAL | 2 | N | 115.64196 | 8.85739 | 2225105 | MASTERSON | 37 | WTP16AARCXP | 2 | N | 138.87933 | 48.23547 | 2225105 | MASTERSON | 38 | WTP15ABYGFC | 2 | N | 200.01633 | 7.71642 | 2225105 | MASTERSON | 39 | WTP16AAPBLL | 2 | N | 331.87413 | 49.516 | 2225105 | MASTERSON | 40 | WTP14ACZRAI | 2 | N | 328.64329 | -70.02436 | 2225105 | MASTERSON | 41 | WTP18AAMPWJ | 2 | N | 26.67683 | 32.50814 | 2225105 | MASTERSON | 42 | WTP15ABUQNJ | 2 | N | 68.732 | -0.69592 | 2225105 | MASTERSON | 43 | WTP14ACKXCR | 2 | N | 48.82067 | -16.43378 | 2225105 | MASTERSON | 44 | WTP19AALJMZ | 2 | N | 359.79663 | 1.16856 | 2225105 | MASTERSON | 45 | WTP18AANJWC | 2 | N | 99.39171 | 69.15233 | 2225105 | MASTERSON | 46 | WTP16AAPTJA | 2 | N | 237.91892 | 8.87392 | 2225105 | MASTERSON | 47 | WTP15AAEPOL | 2 | N | 63.76779 | 36.72397 | 2225105 | MASTERSON | 48 | WTP17AALWZI | 2 | N | 251.97658 | 38.72833 | 2225105 | MASTERSON | 49 | WTP14ADAOYA | 2 | N | 6.97225 | -69.02739 | 2225105 | MASTERSON | 50 | WTP18AADMEZ | 2 | N | 132.54142 | -31.63397 | 2225105 | MASTERSON | 51 | WTP14ACZNJM | 2 | N | 209.62788 | 81.07633 | 2225105 | MASTERSON | 52 | WTP17AAKTRS | 2 | N | 171.19271 | 4.92383 | 2225105 | MASTERSON | 53 | WTP15ACALBW | 2 | N | 99.23825 | 47.03547 | 2225105 | MASTERSON | 54 | WTP16AASFKY | 2 | N | 343.6745 | -27.89692 | 2225105 | MASTERSON | 55 | WTP15ABUYJP | 2 | N | 17.04904 | 85.69742 | 2225105 | MASTERSON | 56 | WTP18AAOMJE | 2 | N | 267.83425 | 52.54569 | 2225105 | MASTERSON | 57 | WTP17AALMRA | 2 | N | 197.31808 | -44.77981 | 2225105 | MASTERSON | 58 | WTP19AANQHX | 2 | N | 336.99354 | 18.32181 | 2225105 | MASTERSON | 59 | WTP15ACBGPN | 2 | N | 166.25825 | 59.68436 | 2225105 | MASTERSON | 60 | WTP19AAKRAI | 2 | N | 314.26237 | 14.20453 | 2225105 | MASTERSON | 61 | WTP15ABYYCQ | 2 | N | 237.48 | 33.46444 | 2225105 | MASTERSON | 62 | WTP17AALBEK | 2 | N | 202.25858 | 23.68569 | 2225105 | MASTERSON | 63 | WTP16AASYCR | 2 | N | 201.93421 | -5.48014 | 2225105 | MASTERSON | 64 | WTP18AAJWVZ | 2 | N | 220.94767 | -39.41497 | 2225105 | MASTERSON | 65 | WTP18AACYGY | 2 | N | 285.23854 | -24.4 | 2225105 | MASTERSON | 66 | WTP14ACTLWY | 2 | N | 6.62358 | 37.64733 | 2225105 | MASTERSON | 67 | WTP15ABYMDQ | 2 | N | 57.21987 | -55.42639 | 2225105 | MASTERSON | 68 | WTP16AAVEUO | 2 | N | 184.78287 | 5.27933 | 2225105 | MASTERSON | 69 | WTP19AAJIKW | 2 | N | 234.22121 | 31.85436 | 2225105 | MASTERSON | 70 | WTP15AASXBN | 2 | N | 115.96896 | -24.84942 | 2225105 | MASTERSON | 71 | WTP15ACCARC | 2 | N | 347.06937 | 37.70294 | 2225105 | MASTERSON | 72 | WTP15ABVPLV | 2 | N | 111.04467 | 27.89961 | 2225105 | MASTERSON | 73 | WTP18AAJKMK | 2 | N | 40.099 | -2.72825 | 2225105 | MASTERSON | 74 | WTP17AALMSG | 2 | N | 222.12063 | 11.62558 | 2225105 | MASTERSON | 75 | WTP17AALZPX | 2 | N | 50.85696 | -2.04678 | 2225105 | MASTERSON | 76 | WTP17AALMSG | 2 | N | 222.12063 | 11.62558 | 2225105 | MASTERSON | 77 | WTP17AANAWB | 2 | N | 137.76208 | -9.62042 | 2225105 | MASTERSON | 78 | WTP17AALQGV | 2 | N | 31.71413 | -11.22822 | 2225105 | MASTERSON | 79 | WTP14ABNPGK | 2 | N | 251.47767 | -23.45175 | 2225105 | MASTERSON | 80 | WTP16AATSNW | 2 | N | 254.84442 | 20.82983 | 2225105 | MASTERSON | 81 | WTP10ACJNVQ | 2 | N | 131.61433 | -59.16278 | 2225105 | MASTERSON | 82 | WTP14ACKODC | 2 | N | 207.02492 | 7.38753 | 2225105 | MASTERSON | 83 | WTP16AAPICT | 2 | N | 26.24958 | 28.09192 | 2225105 | MASTERSON | 84 | WTP14ACZAKM | 2 | N | 96.8225 | -35.21411 | 2225105 | MASTERSON | 85 | WTP16AAUBRH | 2 | N | 274.01183 | 36.614 | 2225105 | MASTERSON | 86 | WTP15ABZMAS | 2 | N | 70.47338 | -39.77547 | 2225105 | MASTERSON | 87 | WTP15ABTXZI | 2 | N | 223.43029 | 27.31717 | 2225105 | MASTERSON | 88 | WTP14ACSTBQ | 2 | N | 351.22067 | 37.21539 | 2225105 | MASTERSON | 89 | WTP15ABXJTH | 2 | N | 10.37329 | -63.15933 | 2225105 | MASTERSON | 90 | WTP17AAKWRK | 2 | N | 190.73071 | 25.62442 | 2225105 | MASTERSON | 91 | WTP17AAMGRX | 2 | N | 269.74142 | 39.86817 | 2225105 | MASTERSON | 92 | WTP14ACHYBJ | 2 | N | 133.39546 | -28.16803 | 2225105 | MASTERSON | 93 | WTP15ABVFJG | 2 | N | 97.325 | 66.79094 | 2225105 | MASTERSON | 94 | WTP14ACYEWQ | 2 | N | 269.97642 | 24.29225 | 2225105 | MASTERSON | 95 | WTP17AAIMNJ | 2 | N | 124.33075 | -24.23733 | 2225105 | MASTERSON | 96 | WTP14ACKVUX | 2 | N | 244.58513 | 52.51406 | 2225105 | MASTERSON | 97 | WTP17AAMZEW | 2 | N | 146.23583 | 31.09794 | 2225105 | MASTERSON | 98 | WTP14ACZAJV | 2 | N | 105.36433 | 59.27106 | 2225105 | MASTERSON | 99 | WTP15ABYIWQ | 2 | N | 19.58429 | -15.26375 | 2225105 | MASTERSON | 100 | WTP17AAMSXP | 2 | N | 126.49067 | 45.2525 | 2225105 | MASTERSON | 101 | WTP16AAQRCR | 2 | N | 280.83067 | -62.11225 | 2225105 | MASTERSON | 102 | WTP14AAMFEK | 2 | N | 85.92067 | 31.70522 | 2225105 | MASTERSON | 103 | WTP14ADAXZI | 2 | N | 156.57913 | 45.578 | 2225105 | MASTERSON | 104 | WTP17AAHSZT | 2 | N | 90.64404 | 49.60322 | 2225105 | MASTERSON | 105 | WTP14ADAQLC | 2 | N | 135.73067 | 19.58358 | 2225105 | MASTERSON | 106 | WTP15ACDELM | 2 | N | 236.40329 | 70.72547 | 2225105 | MASTERSON | 107 | WTP16AATVBU | 2 | N | 260.58358 | 31.74353 | 2225105 | MASTERSON | 108 | WTP16AAVCPT | 2 | N | 11.25213 | -0.78978 | 2225105 | MASTERSON | 109 | WTP17AANBSO | 2 | N | 180.90971 | 58.98656 | 2225105 | MASTERSON | 110 | WTP15ABZDPE | 2 | N | 47.13192 | -0.83603 | 2225105 | MASTERSON | 111 | WTP18AAJQQD | 2 | N | 232.9645 | 37.41275 | 2225105 | MASTERSON | 112 | WTP14ADBJSH | 2 | N | 342.95317 | -20.60803 | 2225105 | MASTERSON | 113 | WTP15ABTYCD | 2 | N | 188.92863 | -47.22739 | 2225105 | MASTERSON | 114 | WTP17AAIOSN | 2 | N | 304.29663 | 58.20253 | 2225105 | MASTERSON | 115 | WTP15AAXNAV | 2 | N | 150.87908 | -44.39189 | 2225105 | MASTERSON | 116 | WTP14ADBQMD | 2 | N | 169.46942 | 29.30453 | 2225121 | BORGHESE | 1 | MAGNETAR OUTBURST | 45 | Y | 0 | 0 | 2225124 | EVANS | 1 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 2 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 3 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 4 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 5 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 6 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 7 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 8 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 9 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 10 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 11 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 12 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 13 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 14 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 15 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 16 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 17 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 18 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 19 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 20 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 21 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 22 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 23 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 24 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 25 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 26 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 27 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 28 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 29 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 30 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 31 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 32 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 33 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 34 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 35 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 36 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 37 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 38 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 39 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 40 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 41 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 42 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 43 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 44 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 45 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 46 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 47 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 48 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 49 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 50 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 51 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 52 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 53 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 54 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 55 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 56 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 57 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 58 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 59 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 60 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 61 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 62 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 63 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 64 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 65 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 66 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 67 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 68 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 69 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 70 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 71 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 72 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 73 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 74 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 75 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 76 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 77 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 78 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 79 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 80 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 81 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 82 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 83 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 84 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 85 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 86 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 87 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 88 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 89 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 90 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 91 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 92 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 93 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 94 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 95 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 96 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 97 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 98 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 99 | TBD TOO | 2.5 | Y | 0 | 0 | 2225124 | EVANS | 100 | TBD TOO | 2.5 | Y | 0 | 0 | 2225125 | DEGENAAR | 1 | GALACTIC CENTER | 490 | N | 266.4 | -28.98333 | 2225128 | LAWTHER | 1 | MRK 590 | 57 | Y | 33.63983 | -0.76672 | 2225129 | DEGENAAR | 1 | VFXT-1 | 25 | Y | 0 | 0 | 2225129 | DEGENAAR | 2 | VFXT-2 | 25 | Y | 0 | 0 | 2225131 | WOODWARD | 1 | T CRB | 28 | Y | 239.87567 | 25.92017 | 2225131 | WOODWARD | 2 | T CRB | 80 | Y | 239.87567 | 25.92017 | 2225131 | WOODWARD | 3 | T CRB | 12 | Y | 239.87567 | 25.92017 | 2225131 | WOODWARD | 4 | T CRB | 26 | Y | 239.87567 | 25.92017 | 2225136 | CHAKRABORTY | 1 | ZTF19ACNSKYY | 150 | N | 203.83271 | 7.46881 | 2225139 | LINCETTO | 1 | KM3NET TOO 1 | 14 | Y | 0 | 0 | 2225139 | LINCETTO | 2 | KM3NET TOO 2 | 14 | Y | 0 | 0 | 2225144 | NUNEZ | 1 | 1.56E+18 | 40 | N | 205.8575 | 56.48044 | 2225144 | NUNEZ | 2 | 1.60E+18 | 40 | N | 219.53708 | 49.99997 | 2225144 | NUNEZ | 3 | 1.61E+18 | 38.1 | N | 221.905 | 51.62792 | 2225144 | NUNEZ | 4 | 1.51E+18 | 36.8 | N | 213.12083 | 47.37925 | 2225144 | NUNEZ | 5 | 1.62E+18 | 8.5 | N | 217.69375 | 60.19036 | 2225144 | NUNEZ | 6 | 1.60E+18 | 9.8 | N | 229.1525 | 54.66819 | 2225144 | NUNEZ | 7 | 1.60E+18 | 13 | N | 236.47667 | 54.69214 | 2225144 | NUNEZ | 8 | 1.39E+18 | 13.8 | N | 244.46375 | 44.78003 | 2225144 | NUNEZ | 9 | 1.40E+18 | 11.2 | N | 234.13475 | 48.27972 | 2225144 | NUNEZ | 10 | 1.40E+18 | 8.6 | N | 240.51 | 51.33531 | 2225144 | NUNEZ | 11 | 1.40E+18 | 24.3 | N | 237.38125 | 50.87058 | 2225144 | NUNEZ | 12 | 1.40E+18 | 9.7 | N | 237.92417 | 52.30631 | 2225144 | NUNEZ | 13 | 1.41E+18 | 3 | N | 240.27833 | 53.41639 | 2225144 | NUNEZ | 14 | 1.41E+18 | 19.4 | N | 251.4525 | 51.21631 | 2225144 | NUNEZ | 15 | 1.41E+18 | 11.6 | N | 253.89083 | 52.87233 | 2225144 | NUNEZ | 16 | 1.42E+18 | 16 | N | 255.73 | 54.34069 | 2225144 | NUNEZ | 17 | 1.43E+18 | 16.4 | N | 242.31042 | 53.4455 | 2225144 | NUNEZ | 18 | 1.50E+18 | 3.5 | N | 211.22792 | 42.92375 | 2225144 | NUNEZ | 19 | 1.51E+18 | 23.8 | N | 209.59917 | 51.37844 | 2225144 | NUNEZ | 20 | 1.51E+18 | 5.5 | N | 208.65208 | 52.01122 | 2225144 | NUNEZ | 21 | 1.51E+18 | 12.4 | N | 211.62167 | 52.98533 | 2225144 | NUNEZ | 22 | 1.56E+18 | 6.5 | N | 207.49292 | 53.24642 | 2225144 | NUNEZ | 23 | 1.56E+18 | 7.9 | N | 201.34 | 52.42244 | 2225144 | NUNEZ | 24 | 1.60E+18 | 6.4 | N | 234.46 | 51.53767 | 2225144 | NUNEZ | 25 | 1.60E+18 | 6.7 | N | 230.81625 | 54.84822 | 2225144 | NUNEZ | 26 | 1.60E+18 | 19.8 | N | 234.45625 | 57.68433 | 2225144 | NUNEZ | 27 | 1.61E+18 | 19.1 | N | 220.73458 | 52.68367 | 2225144 | NUNEZ | 28 | 1.61E+18 | 4.5 | N | 212.16375 | 55.92603 | 2225144 | NUNEZ | 29 | 1.61E+18 | 16.3 | N | 218.89625 | 56.93225 | 2225144 | NUNEZ | 30 | 1.61E+18 | 2 | N | 216.29625 | 57.63319 | 2225144 | NUNEZ | 31 | 1.61E+18 | 10.6 | N | 222.57458 | 58.68911 | 2225144 | NUNEZ | 32 | 1.61E+18 | 1 | N | 225.82 | 59.01153 | 2225144 | NUNEZ | 33 | 1.61E+18 | 7.7 | N | 228.995 | 58.58511 | 2225144 | NUNEZ | 34 | 1.62E+18 | 4 | N | 231.92333 | 59.98703 | 2225144 | NUNEZ | 35 | 1.62E+18 | 8.2 | N | 222.87583 | 59.53208 | 2225144 | NUNEZ | 36 | 1.63E+18 | 12.3 | N | 246.805 | 62.96806 | 2225144 | NUNEZ | 37 | 1.66E+18 | 12.2 | N | 204.86333 | 61.06172 | 2225160 | MARCOTULLI | 1 | LSXPS J151416.5-5808 | 30 | N | 228.56904 | -58.13711 | 2225160 | MARCOTULLI | 2 | LSXPS J085312.5-4322 | 37.5 | N | 133.30242 | -43.37028 | 2225162 | KAPLAN | 1 | VAST 1 | 5 | Y | 0 | 0 | 2225162 | KAPLAN | 2 | VAST 2 | 5 | Y | 0 | 0 | 2225162 | KAPLAN | 3 | VAST 3 | 5 | Y | 0 | 0 | 2225162 | KAPLAN | 4 | VAST 4 | 5 | Y | 0 | 0 | 2225165 | VIELIUTE | 1 | POX 52 | 32.4 | N | 180.73721 | -20.93417 | 2225171 | BODEWITS | 1 | C/2024 E1 | 25.6 | N | 0 | 0 | 2225171 | BODEWITS | 2 | C/2024 T5 | 40 | N | 0 | 0 | 2225173 | BUSON | 1 | BZBJ0630-2406 | 30 | N | 97.748 | -24.113. | 2225175 | DELAUNAY | 1 | GRBS | 5 | Y | 0 | 0 | 2225175 | DELAUNAY | 2 | GRBS | 5 | Y | 0 | 0 | 2225175 | DELAUNAY | 3 | GRBS | 5 | Y | 0 | 0 | 2225175 | DELAUNAY | 4 | GRBS | 5 | Y | 0 | 0 | 2225175 | DELAUNAY | 5 | GRBS | 5 | Y | 0 | 0 | 2225175 | DELAUNAY | 6 | GRBS | 5 | Y | 0 | 0 | 2225175 | DELAUNAY | 7 | GRBS | 5 | Y | 0 | 0 | 2225175 | DELAUNAY | 8 | GRBS | 5 | Y | 0 | 0 | 2225175 | DELAUNAY | 9 | GRBS | 5 | Y | 0 | 0 | 2225175 | DELAUNAY | 10 | GRBS | 5 | Y | 0 | 0 | 2225180 | MASTERSON | 1 | 1ES 1927+654 | 52 | N | 291.83142 | 65.56508 | 2225181 | MILLER | 1 | NGC5273 | 81 | N | 205.53492 | 35.65431 | 2225186 | ARCODIA | 1 | ERO-QPE5 | 63 | N | 51.43 | -45.21219 | 2225188 | ARCODIA | 1 | SDSS J130434.92+0755 | 7.5 | N | 196.14554 | 7.91806 | 2225188 | ARCODIA | 2 | 2MASS 12264436+07330 | 7.5 | N | 186.68483 | 7.55217 | 2225188 | ARCODIA | 3 | SDSS J120850.49+0123 | 7.5 | N | 182.21042 | 1.38931 | 2225194 | LIN | 1 | HLX-1_2MASXJ0111-45 | 36 | N | 17.69583 | -46.02556 | 2225201 | QUIMBY | 1 | SLSN1_VETTING | 3 | Y | 0 | 0 | 2225201 | QUIMBY | 2 | SLSN2_VETTING | 3 | Y | 0 | 0 | 2225201 | QUIMBY | 3 | SLSN3_VETTING | 3 | Y | 0 | 0 | 2225201 | QUIMBY | 4 | SLSN4_VETTING | 3 | Y | 0 | 0 | 2225201 | QUIMBY | 5 | SLSN5_VETTING | 3 | Y | 0 | 0 | 2225201 | QUIMBY | 6 | SLSN6_VETTING | 3 | Y | 0 | 0 | 2225201 | QUIMBY | 7 | SLSN7_VETTING | 3 | Y | 0 | 0 | 2225201 | QUIMBY | 8 | SLSN8_VETTING | 3 | Y | 0 | 0 | 2225201 | QUIMBY | 9 | BRIGHT_SLSN1_LC | 40.5 | Y | 0 | 0 | 2225201 | QUIMBY | 10 | BRIGHT_SLSN2_LC | 40.5 | Y | 0 | 0 | 2225201 | QUIMBY | 11 | FAINT_SLSN3_LC | 23 | Y | 0 | 0 | 2225201 | QUIMBY | 12 | FAINT_SLSN4_LC | 23 | Y | 0 | 0 | 2225205 | SOKOLOSKI | 1 | T CRB | 88 | N | 239.87567 | 25.92017 | 2225208 | ANUMARLAPUDI | 1 | ASKAP VAST TDE 1 | 6 | N | 0 | 0 | 2225208 | ANUMARLAPUDI | 2 | ASKAP VAST TDE 2 | 6 | N | 0 | 0 | 2225208 | ANUMARLAPUDI | 3 | ASKAP VAST TDE 3 | 6 | N | 0 | 0 | 2225208 | ANUMARLAPUDI | 4 | ASKAP VAST TDE 4 | 6 | N | 0 | 0 | 2225208 | ANUMARLAPUDI | 5 | ASKAP VAST TDE 5 | 6 | N | 0 | 0 | 2225208 | ANUMARLAPUDI | 6 | ASKAP VAST TDE 6 | 6 | N | 0 | 0 | 2225208 | ANUMARLAPUDI | 7 | ASKAP VAST TDE 7 | 6 | N | 0 | 0 | 2225208 | ANUMARLAPUDI | 8 | ASKAP VAST TDE 8 | 6 | N | 0 | 0 | 2225208 | ANUMARLAPUDI | 9 | ASKAP VAST TDE 9 | 6 | N | 0 | 0 | 2225208 | ANUMARLAPUDI | 10 | ASKAP VAST TDE 10 | 6 | N | 0 | 0 | 2225216 | STEIN | 1 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 2 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 3 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 4 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 5 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 6 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 7 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 8 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 9 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 10 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 11 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 12 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 13 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 14 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 15 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 16 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 17 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 18 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 19 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 20 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 21 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 22 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 23 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 24 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 25 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 26 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 27 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 28 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 29 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 30 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 31 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 32 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 33 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 34 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 35 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 36 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 37 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 38 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 39 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 40 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 41 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 42 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 43 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 44 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 45 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 46 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 47 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 48 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 49 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 50 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 51 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 52 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 53 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 54 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 55 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 56 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 57 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 58 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 59 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 60 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 61 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 62 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 63 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 64 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 65 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 66 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 67 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 68 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 69 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 70 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 71 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 72 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 73 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 74 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 75 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 76 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 77 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 78 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 79 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 80 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 81 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 82 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 83 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 84 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 85 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 86 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 87 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 88 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 89 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 90 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 91 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 92 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 93 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 94 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 95 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 96 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 97 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 98 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 99 | TOO 1 | 2 | Y | 0 | 0 | 2225216 | STEIN | 100 | TOO 1 | 2 | Y | 0 | 0 | 2225238 | FOLEY | 1 | 2022ACSH | 3.03 | N | 159.26587 | 43.64797 | 2225238 | FOLEY | 2 | 2022AAIQ | 1.97 | N | 216.63338 | 56.58419 | 2225238 | FOLEY | 3 | 2023ALF | 1.26 | N | 207.46333 | -13.20394 | 2225238 | FOLEY | 4 | 2023FTR | 4.3 | N | 139.20817 | 20.17833 | 2225238 | FOLEY | 5 | 2023HRW | 4.02 | N | 204.88725 | 29.99756 | 2225238 | FOLEY | 6 | 2023GRN | 4.2 | N | 151.884 | -12.96058 | 2225238 | FOLEY | 7 | 2023GUY | 4.14 | N | 193.98087 | 7.93067 | 2225238 | FOLEY | 8 | 2023GXF | 4.67 | N | 257.22542 | 19.17236 | 2225238 | FOLEY | 9 | 2023HSW | 4.47 | N | 167.08317 | 10.04306 | 2225238 | FOLEY | 10 | 2023HRO | 4.1 | N | 190.94425 | -20.15822 | 2225238 | FOLEY | 11 | 2023HSY | 4.19 | N | 167.44275 | 11.19256 | 2225238 | FOLEY | 12 | 2023IKS | 5.29 | N | 263.80317 | 6.77458 | 2225238 | FOLEY | 13 | 2023JWW | 4.91 | N | 269.84312 | 17.26008 | 2225238 | FOLEY | 14 | 2023JVU | 4.74 | N | 249.50267 | 55.40508 | 2225238 | FOLEY | 15 | 2023JWR | 4.86 | N | 229.27754 | 11.36406 | 2225238 | FOLEY | 16 | 2023KMJ | 4.04 | N | 225.11517 | 6.45456 | 2225238 | FOLEY | 17 | 2023MDE | 5.26 | N | 257.85513 | 13.56919 | 2225238 | FOLEY | 18 | 2023EXT | 3.95 | N | 165.01496 | 8.16678 | 2225238 | FOLEY | 19 | 2023HWM | 4.63 | N | 168.59712 | 53.19942 | 2225238 | FOLEY | 20 | 2023HUY | 4.01 | N | 198.96154 | -16.20508 | 2225238 | FOLEY | 21 | 2023OLS | 4.08 | N | 301.78646 | -0.99561 | 2225238 | FOLEY | 22 | 2023ONO | 4.48 | N | 43.60767 | -22.50258 | 2225238 | FOLEY | 23 | 2023MKT | 4.04 | N | 229.56142 | -24.08675 | 2225238 | FOLEY | 24 | 2022XKQ | 4.6 | N | 76.34879 | -11.88222 | 2225238 | FOLEY | 25 | 2023BEE | 8.42 | N | 134.04846 | -3.32556 | 2225238 | FOLEY | 26 | 2023NLK | 4.72 | N | 260.22204 | 22.20978 | 2225238 | FOLEY | 27 | 2023VPD | 4.06 | N | 340.05379 | 19.50683 | 2225238 | FOLEY | 28 | 2023VER | 4.05 | N | 57.91783 | -0.51083 | 2225238 | FOLEY | 29 | 2023XQN | 3.95 | N | 2.04217 | 27.00367 | 2225238 | FOLEY | 30 | 2023WUK | 7.26 | N | 334.87662 | 29.38822 | 2225238 | FOLEY | 31 | 2023XLR | 1 | N | 8.90825 | 45.93142 | 2225238 | FOLEY | 32 | 2023VYL | 4.23 | N | 350.12363 | 17.22122 | 2225238 | FOLEY | 33 | 2023MVL | 4.18 | N | 295.41867 | -21.26269 | 2225238 | FOLEY | 34 | 2024AXD | 4.53 | N | 75.05087 | -11.34786 | 2225238 | FOLEY | 35 | 2022ZUT | 3.61 | N | 175.24508 | 11.46969 | 2225238 | FOLEY | 36 | 2023XQM | 4.98 | N | 158.64579 | -27.65092 | 2225238 | FOLEY | 37 | 2024GY | 4.02 | N | 183.96371 | 13.11558 | 2225241 | WALTON | 1 | NGC2283 ULX1 | 120 | N | 101.47325 | -18.20114 | 2225243 | TROJA | 1 | SBO-X | 15 | Y | 0 | 0 | 2225243 | TROJA | 2 | SBO-X | 15 | Y | 0 | 0 | 2225243 | TROJA | 3 | SBO-X | 15 | Y | 0 | 0 | 2225243 | TROJA | 4 | SBO-X | 15 | Y | 0 | 0 | 2225243 | TROJA | 5 | SBO-X | 15 | Y | 0 | 0 | 2225244 | DESAI | 1 | ATLASJ0426-5025 | 5 | N | 66.67508 | -50.43186 | 2225244 | DESAI | 2 | GALEX J161854.1-355 | 5 | N | 244.72542 | -35.90742 | 2225244 | DESAI | 3 | GALEX J001536.9-2917 | 5 | N | 3.90375 | -29.28528 | 2225244 | DESAI | 4 | HBQS 0054-3403 | 4.5 | N | 14.10417 | -33.79508 | 2225244 | DESAI | 5 | GALEX J052449.7-3020 | 4.5 | N | 81.20833 | -30.33911 | 2225244 | DESAI | 6 | ZTFJ0118-0156 | 3 | N | 19.54308 | -1.93678 | 2225244 | DESAI | 7 | ZTFJ1828+3459 | 3 | N | 277.23217 | 34.99519 | 2225244 | DESAI | 8 | ZTFJ0214-1212 | 5 | N | 33.53887 | -12.20078 | 2225244 | DESAI | 9 | ZTFJ1852+1520 | 4.5 | N | 283.21733 | 15.33706 | 2225244 | DESAI | 10 | WDJ1328+5908 | 5 | N | 202.24175 | 59.1475 | 2225244 | DESAI | 11 | ZTFJ0005-1002 | 5 | N | 1.48329 | -10.037 | 2225244 | DESAI | 12 | ZTFJ2204+2543 | 3 | N | 331.20404 | 25.71869 | 2225244 | DESAI | 13 | WDJ1042+2030 | 4.5 | N | 160.57975 | 20.50219 | 2225244 | DESAI | 14 | WDJ1557+0411 | 4.5 | N | 239.2835 | 4.19903 | 2225244 | DESAI | 15 | WDJ1351+5419 | 3 | N | 207.92075 | 54.32989 | 2225244 | DESAI | 16 | WD2010+310 | 1.5 | N | 303.09296 | 31.23067 | 2225244 | DESAI | 17 | WDJ0250-0437 | 5 | N | 42.50738 | -4.61753 | 2225244 | DESAI | 18 | WDJ0211+2115 | 3 | N | 32.95133 | 21.26328 | 2225244 | DESAI | 19 | WDJ1034+0327 | 3 | N | 158.62562 | 3.46003 | 2225244 | DESAI | 20 | ZTFJ1719-1446 | 3 | N | 259.83325 | -14.778 | 2225244 | DESAI | 21 | ZTFJ1543+3021 | 3 | N | 235.81262 | 30.35958 | 2225244 | DESAI | 22 | ZTFJ1039-0325 | 3 | N | 159.92292 | -3.42625 | 2225244 | DESAI | 23 | WDJ1020+3626 | 1.8 | N | 155.22529 | 36.446 | 2225244 | DESAI | 24 | WDJ1508+2150 | 4.5 | N | 227.04075 | 21.84364 | 2225244 | DESAI | 25 | WD0945+245. | 1.5 | N | 147.194 | 24.35669 | 2225244 | DESAI | 26 | ZTFJ2041+3808 | 5 | N | 310.29858 | 38.14786 | 2225244 | DESAI | 27 | WDJ2149-0728 | 4.5 | N | 327.378 | -7.47008 | 2225244 | DESAI | 28 | WDJ1427+3721 | 5 | N | 216.76367 | 37.35286 | 2225244 | DESAI | 29 | WD1043-050 | 3 | N | 161.54038 | -5.30431 | 2225244 | DESAI | 30 | J1144+1717 | 4.5 | N | 176.17362 | 17.28772 | 2225244 | DESAI | 31 | WDJ0608-4515 | 5 | N | 92.22321 | -45.25869 | 2225244 | DESAI | 32 | WD0253+508 | 1.8 | N | 44.34167 | 51.06214 | 2225244 | DESAI | 33 | WD0159-032 | 4.5 | N | 30.43188 | -3.03336 | 2225244 | DESAI | 34 | WD1533-057 | 1.8 | N | 234.1455 | -5.87769 | 2225244 | DESAI | 35 | J0257+5103 | 1.8 | N | 44.34167 | 51.06214 | 2225244 | DESAI | 36 | WD0301+059 | 1.8 | N | 45.96171 | 6.13044 | 2225244 | DESAI | 37 | WD0041-102 | 1.5 | N | 10.94096 | -10.00753 | 2225244 | DESAI | 38 | WD1008-242 | 1.8 | N | 152.69908 | -24.45328 | 2225244 | DESAI | 39 | WDJ1407+3011 | 5.5 | N | 211.96096 | 30.19169 | 2225244 | DESAI | 40 | WDJ1133+5152 | 4.5 | N | 173.49008 | 51.86794 | 2225244 | DESAI | 41 | J1707+3532 | 3 | N | 256.96617 | 35.54461 | 2225244 | DESAI | 42 | WD0446-789 | 1 | N | 70.94192 | -78.86392 | 2225244 | DESAI | 43 | ZTFJ0006+3104 | 4.5 | N | 1.65808 | 31.07097 | 2225244 | DESAI | 44 | WD1211-171 | 4.5 | N | 183.53433 | -17.41189 | 2225244 | DESAI | 45 | SDSSJ0935+4429 | 5 | N | 143.75862 | 44.49461 | 2225244 | DESAI | 46 | J1348+3810 | 4.5 | N | 207.08662 | 38.17147 | 2225244 | DESAI | 47 | WD1440+753 | 1.8 | N | 220.02021 | 75.09283 | 2225244 | DESAI | 48 | WDJ0343+1029 | 3 | N | 55.80988 | 10.49392 | 2225244 | DESAI | 49 | ZTFJ0353+0956 | 4.5 | N | 58.31558 | 9.94261 | 2225244 | DESAI | 50 | ZTFJ0718P3731 | 3.5 | N | 109.56825 | 37.52742 | 2225244 | DESAI | 51 | ZTFJ1808+4622 | 3 | N | 272.13904 | 46.369 | 2225249 | LUNDY | 1 | 4C +42.22 | 25 | N | 104.04442 | 42.61742 | 2225252 | CLARK | 1 | HGGK681 | 37.9 | N | 210.8025 | 54.59494 | 2225252 | CLARK | 2 | NGC5471 | 6 | N | 211.11929 | 54.398 | 2225255 | BROWN | 1 | HOST-SN2023ZEU | 3 | N | 24.20521 | 1.58492 | 2225255 | BROWN | 2 | HOST-SN2023ZAZ | 3 | N | 59.73092 | -26.05744 | 2225255 | BROWN | 3 | HOST-SN2023XXJ | 3 | N | 162.58796 | -33.40122 | 2225255 | BROWN | 4 | HOST-SN2023XRS | 3 | N | 41.41604 | -20.80994 | 2225255 | BROWN | 5 | HOST-SN2023XQN | 3 | N | 2.04217 | 27.00367 | 2225255 | BROWN | 6 | HOST-SN2023XNL | 3 | N | 141.62371 | -14.52881 | 2225255 | BROWN | 7 | HOST-SN2023XGO | 3 | N | 76.07996 | 67.62256 | 2225255 | BROWN | 8 | HOST-SN2023XGG | 3 | N | 20.94733 | 30.76506 | 2225255 | BROWN | 9 | HOST-SN2023VYL | 3 | N | 350.12363 | 17.22122 | 2225255 | BROWN | 10 | HOST-SN2023VPE | 3 | N | 46.52858 | 16.25544 | 2225255 | BROWN | 11 | HOST-SN2023VPD | 3 | N | 340.05379 | 19.50681 | 2225255 | BROWN | 12 | HOST-SN2023VER | 3 | N | 57.91779 | -0.51081 | 2225255 | BROWN | 13 | HOST-SN2023VEK | 3 | N | 5.65121 | -24.46233 | 2225255 | BROWN | 14 | HOST-SN2023UTC | 3 | N | 137.99658 | 53.71733 | 2225255 | BROWN | 15 | HOST-SN2023TSZ | 3 | N | 129.373 | -0.04325 | 2225255 | BROWN | 16 | HOST-SN2023TDE | 3 | N | 265.62063 | 39.31861 | 2225255 | BROWN | 17 | HOST-SN2023SFL | 3 | N | 20.16246 | 32.23733 | 2225255 | BROWN | 18 | HOST-SN2023RZY | 3 | N | 18.75021 | 1.69353 | 2225255 | BROWN | 19 | HOST-SN2023RYF | 3 | N | 338.93233 | -8.2295 | 2225255 | BROWN | 20 | HOST-SN2023RKG | 3 | N | 327.393 | -22.12181 | 2225255 | BROWN | 21 | HOST-SN2023RAU | 3 | N | 5.23017 | -1.75792 | 2225255 | BROWN | 22 | HOST-SN2023QDI | 3 | N | 10.32475 | -14.23092 | 2225255 | BROWN | 23 | HOST-SN2023PLG | 3 | N | 109.26317 | 24.95881 | 2225255 | BROWN | 24 | HOST-SN2023PBK | 3 | N | 43.39858 | -35.70789 | 2225255 | BROWN | 25 | HOST-SN2023OZO | 3 | N | 244.77104 | -1.90708 | 2225255 | BROWN | 26 | HOST-SN2023ONO | 3 | N | 43.60762 | -22.50269 | 2225255 | BROWN | 27 | HOST-SN2023OLS | 3 | N | 301.78646 | -0.99564 | 2225255 | BROWN | 28 | HOST-SN2023NLK | 3 | N | 260.22208 | 22.20978 | 2225255 | BROWN | 29 | HOST-SN2023ACHA | 3 | N | 251.21592 | 52.76706 | 2225255 | BROWN | 30 | HOST-SN2024FA | 3 | N | 36.25571 | -24.78689 | 2225255 | BROWN | 31 | HOST-SN2024GY | 3 | N | 183.96379 | 13.10731 | 2225255 | BROWN | 32 | HOST-SN2024UJ | 3 | N | 166.95429 | -20.02619 | 2225255 | BROWN | 33 | HOST-SN2023VBG | 3 | N | 115.9325 | 34.375. | 2225255 | BROWN | 34 | HOST-SN2024DY | 3 | N | 161.68758 | 29.90939 | 2225255 | BROWN | 35 | HOST-SN2023ZGO | 3 | N | 132.22871 | 31.78361 | 2225255 | BROWN | 36 | HOST-SN2024WS | 3 | N | 127.1945 | 73.75239 | 2225255 | BROWN | 37 | HOST-SN2024UJ | 3 | N | 166.9545 | -20.02619 | 2225255 | BROWN | 38 | HOST-SN2024AHV | 3 | N | 244.693 | 7.4125 | 2225255 | BROWN | 39 | HOST-SN2024KA | 3 | N | 181.04071 | 1.826 | 2225255 | BROWN | 40 | HOST-SN2024TV | 3 | N | 126.144 | -22.96969 | 2225255 | BROWN | 41 | HOST-SN2023YPT | 3 | N | 30.97508 | -9.41461 | 2225255 | BROWN | 42 | HOST-SN2023ACFT | 3 | N | 78.7715 | -34.40111 | 2225255 | BROWN | 43 | HOST-SN2024BCH | 3 | N | 78.7715 | -34.40111 | 2225255 | BROWN | 44 | HOST-SN2024CLD | 3 | N | 237.59 | 18.93919 | 2225255 | BROWN | 45 | HOST-SN2024AS | 3 | N | 151.27629 | 17.48919 | 2225255 | BROWN | 46 | HOST-SN2024AS | 3 | N | 151.27629 | 17.48919 |
Proposal Abstracts
2225013 / GRUPE / NORTHERN KENTUCKY UNIVERSITY
"UNDERSTANDING AGN VARIABILITY WITH RESPECT TO AGN PROPERTIES"
The primary goal of this proposal is to identify AGN in extreme X-ray flux states. Swift will re-observe a well-established sample of 120 AGN that will then allow to trigger the most extreme cases of variability (brightest outbursts, deepest fades, strongest spectral changes) among this sample that will be selected for multi-wavelength spectroscopic follow-ups with ground- and space-based observatories through pre-approved ToO programs. In addition, this legacy sample of AGN enables us to measure the variability of each AGN and correlate this with other AGN properties such as black hole mass and Eddington ratio (L/L_{Edd}). Such an approach is only possible with long-term, repeated, simultaneous broad-band optical--UV--X-ray coverage.
2225035 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
"SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS IN CYCLE 22"
We propose to use Swift to localize Galactic X-ray transients discovered by MAXI. MAXI scans almost the entire X-ray sky every ~92 minutes, with a source detection sensitivity of ~60 mCrab in one orbit and ~15 mCrab in one day, discovering X-ray transients with 0.1-0.5 degree accuracies in the 2-20 keV energy band. Swift provides rapid follow-up of MAXI triggers and localization up to 1.4 error radius, which is vital for identifying any optical/radio counterpart. XRT observations will also provide measurements of the low energy X-ray spectra. UVOT data will provide astrometric corrections and possibly optical counterparts. Swift is proven to be uniquely capable in this task.
2225037 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
"RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS IN CYCLE 22"
We seek to identify high-energy counterparts to Fast Radio Bursts, for which the progenitor systems and emission mechanism remain unknown. We propose extremely rapid response follow-up observations with XRT and UVOT for exceptionally bright and low dispersion measure (nearby) events and to save the BAT event data when the FRB position is within the BAT FOV. This proposal takes advantage of new enhancements to Swift's fast-response capability, trigger on CHIME and other detected FRBs within seconds of detection, providing the earliest and deepestconstraints on non-radio emission from FRBs, as well as the greatest chance of finding a counterpart. This will significantly enhance the science return of Swift, and help solve the mystery of FRBs.
2225040 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
"IDENTIFYING THE ELECTROMAGNETIC COUNTERPARTS TO COSMIC NEUTRINO SOURCES"
Swift is a powerful facility for multi-messenger astronomy, having identified the first EM counterparts to both high-energy neutrino and gravitational wave events. We propose to observe the 90% error regions of well-localised neutrinos with a high probability of cosmological origin detected by IceCube and, for the first time, KM3NeT. We request a total of 55.5 ks of approved ToO time.
2225050 / HOLWERDA / UNIVERSITY OF LOUISVILLE
"THE DUST ATTENUATION LAW IN OVERLAPPING GALAXY PAIRS"
How interstellar dust attenuates starlight with wavelength is fundamental to our understanding of galaxies. In the ultraviolet, the Milky Way dust attenuation shows a bump, while other attenuation relations do not. This bump is thought to be due to Polycyclic Aromatic Hydrocarbons (PAHs). The attenuation relation can be measured directly in images of overlapping galaxy pairs, using the symmetry of both galaxies. We ask for SWIFT ultraviolet observations of suitable 30 overlapping galaxy pairs to test the variance in attenuation relations in other spiral galaxies, specifically the reddening slopes and the strength of the 2100A bump. SWIFT W2 maps the 2100A bump strength and WISE W3 PAH emission, allowing us to directly test the PAH hypothesis for the bump feature.
2225056 / MARGUTTI / UNIVERSITY OF CALIFORNIA (BERKELEY)
"XRT+NUSTAR PROMPT OBSERVATIONS OF STRONG SN SHOCK INTERACTION"
Recent observations have revolutionized our understanding of mass loss in evolved massive stars. Contrary to theoretical expectations, observations revealed a rich phenomenology and the ejection of shells of material in the years before explosion. The physical mechanism behind impulsive mass ejections synchronized with core-collapse is unclear. Building on the recent success with SNe 2023ixf and 2024ggi, we propose a coordinated XRT-NuSTAR effort to constrain the early evolution of the soft and hard X-ray spectrum of 1 young nearby (d<20 Mpc) or X-ray bright (Fx>5x10^-14 erg/s/cm2) strongly interacting SN. These observations will characterize the innermost circumstellar medium at times when the radio emission is completely absorbed, revealing the most extreme mass loss histories.
2225061 / MARCULEWICZ / WAYNE STATE UNIVERSITY
"THE MISSING PIECE OF REVERBERATION MAPPING - LOW-MASS AGN NGC 4051"
A key question in AGN studies is the nature of the poorly understood accretion flow. NGC 4051 offers a rare opportunity to observe this process around a low-mass AGN, notable for being one of the brightest examples of its class. Its unique combination of variability, small black hole mass, and accessibility to monitoring makes it an ideal laboratory for testing models of the innermost disc structure, variability mechanisms, and BLR diffuse continuum emission. Building on past campaigns, our proposed Swift monitoring will enable the most comprehensive broadband reverberation mapping of NGC 4051 to date. With unique UV coverage that no other mission can offer, we can probe the structure and physics of the inner flow, providing new insight into accretion in low-mass AGN.
2225066 / SAIKIA / YALE UNIVERSITY
"OBSERVING THE EARLY RISE OF X-RAY TRANSIENTS WITH SWIFT"
Observing campaigns of black hole and neutron star X-ray transients have long relied on triggers from X-ray all-sky monitors or wide-field cameras. Due to the limited sensitivity of these instruments, the early rising phase of outbursts is typically missed. Here we propose a Swift monitoring program of known transient LMXBs that is triggered by detections of optical outburst activity with the Faulkes Telescopes/XB-NEWS. This allows us to catch transients as they emerge from quiescence in UV and X-rays. Our aim is to test the disk-instability model in LMXBs, follow the early X-ray spectral/variability evolution of an outburst, and search for signs of extended absorbing structures. We request monitoring campaigns for two transients, each with 10 (2 ks) observations at a 2-day cadence.
2225067 / HERNANDEZ SANTISTEBAN / UNIVERSITY OF ST. ANDREWS
"UNDERSTANDING AGN VARIABILITY WITH FAIRALL 9: A LEGACY SPECTROSCOPIC ECHO-MAPPING EXPERIMENT WITH SWIFT AND HST"
We propose daily 1ks Swift monitoring of the X-ray bright, unobscured AGN, Fairall 9 to support a 31-HST orbit spectroscopic reverberation mapping experiment spanning 5 months at a 4 day cadence. Our aims are 1) to determine the origin of the reverberating components, quantifying the compact accretion disk and the more extended inner wind and broad-line regions and thereby resolve the puzzle of light travel time lags and inferred accretion disk sizes being larger than expected from theory; 2) to determine the relationship between X-ray and UV-optical variations. This Swift+HST campaign will provide a legacy dataset to explore the fundamental variability mechanisms and give a template to interpret future continuum reverberation mapping experiments (e.g., LSST) on higher-redshift AGN.
2225071 / RAJGURU / CLEMSON UNIVERSITY
"HUNTING EXTREME BLAZARS USING SWIFT-XRT"
We have detected 4 new MeV blazar candidates in the 4th Fermi-LAT AGN catalog (4LAC) that lack 2-10 keV data. These powerful MeV blazars, and other sources detected in the catalog, will pave the way to the exploration of the MeV sky in anticipation of COSI. We request to observe the 4 sources with Swift for a total of 30 ks. The XRT observations will let us detect the proposed sources in the soft X-ray band, accurately measure the spectral shape and flux in this band, and to sample the onset of the inverse Compton emission. These properties are fundamental to determining the power of the jet and to deriving the shape of the underlying electron population responsible for the emission. Measuring the accretion disk emission with UVOT will reveal the disk luminosity and the black hole mass.
2225073 / SALA / UNIVERSITAT POLITECNICA DE CATALUNYA
"MAGNETIC NOVAE: TWO NEW IP CANDIDATES AMONG HISTORICAL NOVAE"
Nova explosions are thermonuclear events that occur on the surface of accreting white dwarfs in cataclysmic variables. Only a few novae have been identified in magnetic systems, and the number of well-studied cases remains small. The role of the white dwarf magnetic field in the nova explosion and the impact of the eruption on the long-term accretion history remain poorly constrained. The eROSITA All-Sky Survey has revealed two old novae, AT~Cnc and RR~Cha, with strong indications of magnetic accretion. This program requests 20 ks per target with Swift/XRT in PC mode, plus UVOT using the Filter of the Day, to confirm the magnetic nature of these systems and characterize their accretion properties.
2225074 / BENOIT / UNIVERSITY OF MINNESOTA
"LOW-LATENCY ALERTS FROM GRAVITATIONAL WAVE SIGNALS FOR SWIFT FOLLOW-UP"
We propose the development of software infrastructure to deliver ultra low-latency gravitational wave (GW) alerts directly to the Swift Observatory. GWs from the coalescence of binary neutron stars (BNS) may be accompanied by kilonovae, and early UV measurements can provide unique insights. The time from the merger of a compact binary to the production of sky-maps is approximately 30 seconds for existing search pipelines within the LIGO-Virgo-KAGRA Collaboration. However, advances in machine learning search pipelines have been able to reduce this latency to 12-15 seconds. We will: (1) develop these pipelines to enable early-warning detection of BNS mergers; (2) reduce latencies that exist within the online search; and (3) communicate detections directly to Swift for potential follow-up.
2225085 / SRINIVASARAGAVAN / UNIVERSITY OF MARYLAND (COLLEGE PARK)
"FOLLOW UP X-RAY OBSERVATIONS OF X-RAY FLASH CANDIDATES DURING SWIFT CYCLE 22"
The Einstein Probe (EP) and Space-based multi-band astronomical Variable Objects Monitor (SVOM) are beginning to find X-ray Flashes (XRFs), bursts with peak energies less than classical long gamma-ray bursts (LGRBs). Their properties are currently unknown - some theories suggest they may be off-axis LGRBs, while others suggest they are a new class of phenomena altogether. Their X-ray afterglows are a key part of their emission, as they are essential for analyzing the properties of their non-thermal emitting ejecta. Therefore, we propose to observe the X-ray afterglows of XRF candidates discovered by EP and SVOM during \textit{Swift} Cycle 22, in order to build the first flux-limited sample of EP and SVOM XRF X-ray afterglows.
2225086 / VASYLYEV / UNIVERSITY OF CALIFORNIA (SAN DIEGO)
"ULTRA-RAPID, HIGH-CADENCE UV PHOTOMETRY OF INFANT SUPERNOVAE"
SNe discovered within a day of explosion probe several poorly understood stellar evolutionary processes. Core-collapse SNe reveal nearby CSM that is quickly swept up by the ejecta, and some SNe Ia show an early light-curve excess that has been attributed to collision with a binary companion, detonation of the WD's helium shell, or CSM interaction. UV observations uniquely constrain all these phenomena, but they evolve over hours and disappear after days. We propose to obtain 6 h-cadence UV light curves, starting <1 h after discovery and lasting for 3 d, of up to 5 nearby infant SNe. This program will leverage Swift's unique time-domain UV abilities to grow the small sample of SNe observed during these early phases and strongly constrain their progenitor systems and explosion physics.
2225087 / WILSON / UNIVERSITY OF COLORADO AT BOULDER
"NUV PHOTOMETRY OF THE MOST LIKELY TARGETS FOR THE HABITABLE WORLDS OBSERVATORY"
The HWO mission is being designed to return spectra of truly Earth like-planets. A vital missing piece of the puzzle are the NUV fluxes of the host stars, which will enable us to predict the reflectance spectra for Earth analogs and thus the spectra that HWO must be designed to measure. UVOT/UVM2 photometry is the ideal measurement to fulfill this requirement. With 36 bright targets and no timing constraints, we submit this as a fill-in proposal. In perhaps its final year, Swift data will enable the design of the next Great Observatory.
2225100 / CHAKRABORTY / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"UNDERSTANDING THE DIVERSITY OF LATE-TIME BEHAVIOR IN TIDAL DISRUPTION EVENTS"
The canonical picture of Tidal Disruption Events (TDEs) suggests the soft X-ray emission rises on timescales of ~1 month then declines as t^-5/3, but in recent years, Swift, eROSITA, and NICER monitoring has revealed they often do not follow this simple prescription. A growing handful of TDEs have shown unexpected X-ray behaviors at late times, including late-time brightening, spectral hardening, X-ray plateaus, and high-amplitude variability/Quasi-Periodic Eruptions (QPEs). Discovery is made difficult by the sparse coverage at late times; we aim to correct this bias with a fill-in proposal to obtain updated late-time X-ray/UV flux measurements of all previously detected TDEs and systematically determine the ubiquity of unexpected late-time X-ray behavior.
2225105 / MASTERSON / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"A LATE-TIME X-RAY VIEW OF MID-INFRARED-SELECTED TDE CANDIDATES"
Recent works searching for mid-infrared (MIR) nuclear transients have revealed a number of TDEs in nearby star-forming galaxies. The majority of these TDEs have shown no optical counterpart, suggesting that these samples represent a new, historically-overlooked TDE population. A handful of these sources show variable X-ray emission associated with the formation of an accretion disk. We propose Swift fill-in observations of a sample of 116 MIR-selected TDE candidates out to z = 0.1. With this sample, we will constrain the true detection fraction of late-time X-ray emission and probe the X-ray spectral variability and line-of-sight absorption in this new TDE population.
2225121 / BORGHESE / EUROPEAN SPACE ASTRONOMY CENTRE (ESAC)
"SWIFT MONITORING OF MAGNETAR OUTBURSTS"
Powered by the instabilities and decay of their huge magnetic field, magnetars are characterized by a distinctive high-energy flaring phenomenology: short bursts of X-/gamma-rays, often accompanied by enhancements of the persistent X-ray luminosity, referred to as outbursts. Magnetar-like activity was detected from isolated neutron stars with a broad range of magnetic field strengths. Moreover, the detection of a fast radio burst-like burst from a Galactic magnetar has proved that at least a sub-group of fast radio bursts can be powered by magnetars. We propose to follow one outburst from a known or new magnetar with Swift during the first months to gather new physical insights on magnetars surface, field configuration and magnetosphere.
2225124 / EVANS / UNIVERSITY OF LEICESTER
"FOLLOW UP OF NEW X-RAY TRANSIENTS DETECTED BY SWIFT"
The 'Living Swift-XRT Point Source Catalogue' (LSXPS) identifies and reports serendipitous transients in Swift-XRT data in near real-time. This allows for rapid, multi-wavelength follow up, the value of which was shown by the first ever discovery of nuclear quasi-periodic eruptions with a timescale of ~a month. To date, only a small number of transient candidates from LSXPS have been followed up rapidly, though recent work shows that the contamination from sources upscattered by the Eddington Bias is much lower than previously thought. We propose to systematically follow up transients discovered by LSXPS across X-ray, UV and optical wavelengths, to classify the events, constrain their physics, and motivate follow up with other facilities and wavelengths.
2225125 / DEGENAAR / UNIVERSITEIT VAN AMSTERDAM
"TOWARDS TWO DECADES OF SWIFT MONITORING OF THE GALACTIC CENTER"
The center of our Galaxy has been monitored with the Swift/XRT almost every day since 2006. The high cadence provides excellent means to capture X-ray flares from Sgr A*, to study the accretion properties of 18 transient X-ray binaries, and to discover new X-ray transients. We propose to continue this Swift legacy program in cycles 22-23 and request daily 1-ks observations that amount to 490 ks of total exposure time. Our main objectives are to: 1) collect and study new flares from Sgr A*, 2) to detect any changes in the flaring rate or persistent emission of the supermassive black hole, and 3) to apply accretion models to very-faint X-ray binaries to determine their disk sizes. Many other topics can be addressed by this program, so it is highly valuable for a broad community.
2225128 / LAWTHER / UNIVERSITY OF ARIZONA
"CAPTURING THE CONTINUED EVOLUTION OF AN EXTREME AGN"
Mrk 590 is an extremely variable AGN that fully re-ignited during 2024, after several years of low-level X-ray--driven flaring. To probe the physics of its accretion flow and broad-line region, we ask to monitor Mrk 590 with Swift every four days for a 152-day (i.e., 38-visit; 57 ks total) ToO monitoring run if its UV brightness changes significantly during Cycle 22. We will determine the evolution of the ionizing continuum source, and obtain a reverberation mapping measurement of the surrounding broad-line gas. This ToO campaign will supplement an on-going Swift/VLT reverberation mapping campaign (Cycle 21, priv.comm.), providing crucial additional insight into how changes in the accretion rate influence the continuum emission and its feedback on the environment around the black hole.
2225129 / DEGENAAR / UNIVERSITEIT VAN AMSTERDAM
"THE NATURE AND ACCRETION FLOW PROPERTIES OF SUB-LUMINOUS X-RAY BINARIES"
Very-faint X-ray transients exhibit accretion outbursts with a peak X-ray luminosity much lower than that of other black hole and neutron star X-ray binaries. These objects trace a poorly understood accretion regime and may represent a missing population of short-period binaries or neutron stars that act as magnetic propellers. We propose 50 ks of Swift ToO monitoring and 14h of VLA radio observations to study the outbursts of two very-faint X-ray transients. These data are complemented by optical monitoring with rapidly schedulable 1-2 m telescopes and nIR spectroscopy with 8-m class telescopes. We aim to study the properties of their accretion in/outflow, elucidate the nature of individual sources, and ultimately determine the fractions of different types of systems among the population.
2225131 / WOODWARD / UNIVERSITY OF MINNESOTA
"WAITING FOR GODOT - THE SWIFT T CORONAE BOREALIS REVEAL"
T Coronae Borealis (T CrB), a symbiotic recurrent nova (RN) that is expected to erupt imminently after a hiatus of over 80 yrs has never been studied in the X-ray/UV during outburst. This proposal's goal during AO22 is to obtain high S/N, high cadence and multi-wavelength Swift observations during, and after the next eruption of what is expected to be the brightest x-ray emitting nova since 1946. Swift's unique x-ray and UV capabilities will provide the necessary data to estimate the white dwarf mass and the ejecta mass, which when compared with the mass accretion rate during quiescence, constitute the critical parameters that will determine the fate of this prime candidate for a SN Ia progenitor.
2225136 / CHAKRABORTY / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"MONITORING THE EXTREME QUASI-PERIODIC ERUPTIONS IN ZTF19ACNSKYY"
Quasi-Periodic Eruptions (QPEs) are luminous (L~10^41-44 erg/s) recurring (2 to 250 hrs) soft X-ray transients from supermassive black holes (SMBHs). Leading models invoke the extreme mass-ratio inspiral (EMRI) of a solar mass companion colliding with the SMBH accretion disk. This carries the exciting implication that QPEs may be the first-observed counterparts to EMRIs in advance of upcoming space-based interferometers (e.g. LISA) which will directly detect their gravitational-wave signatures. Of the dozen known QPE sources, ZTF19acnskyy ( Ansky ) is the most extreme in its timescales and energetics, pushing EMRI models to their limits. Here we propose a 75-day, 150 ks Swift UVOT/XRT monitoring campaign of Ansky.
2225139 / LINCETTO / UNIVERSITAT WURZBURG
"SWIFT FOLLOW UP OF KM3NET HIGH-ENERGY NEUTRINO EVENTS"
A diffuse flux of high-energy neutrinos of astrophysical origin in the TeV-PeV energy range has been observed by the IceCube Neutrino Observatory. While several candidate neutrino sources exist, the majority of the flux remains unexplained. The KM3NeT Collaboration is building a network of Cherenkov neutrino detectors in the Mediterranean Sea and has started a realtime program able to promptly select and reconstruct neutrinos of likely astrophysical origin with a containment radius within 1 deg. The program aims to follow up to two neutrinos with energy above 100 TeV that will be detected by KM3NeT in the observation period.
2225144 / NUNEZ / COLUMBIA UNIVERSITY
"CONTINUING THE X-RAY CENSUS OF GROUP-X, A NEW LABORATORY FOR INVESTIGATING THE ACTIVITY-ROTATION RELATION"
Open clusters are great laboratories for examining the dependence of magnetic activity on rotation for low-mass stars (<1.3 Solar mass). For potentially habitable Earth-like planets, likely to be discovered orbiting such stars, it is essential to understand the high-energy environments in which they form. We propose to continue the observations of 41 low-mass members of Group-X (~100 pc away and ~300 Myr old), which were partially observed as part of the Fill-in Program in Cycles 20 and 21. We used light curves from optical surveys to measure rotation periods for all these low-mass members of the cluster. Our Swift data will make Group-X a critical new benchmark as we seek to map out the magnetic behavior of low-mass stars over their first 1 Gyr.
2225160 / MARCOTULLI / CLEMSON UNIVERSITY
"UNVEILING THE NATURE OF NEWLY DETECTED MEV GALACTIC SOURCES"
We propose to observe 2 new candidates MeV emitting Galactic sources with XRT for a total of 67.5ks. These sources have been detected for the very first time in the 20-200 MeV range and reside in the Galactic plane (|b|<5 deg). However, the lack of good-quality X-ray data hampers the source classification (e.g. SNR, PSR, PWN), and the characterization of their spectral properties (spectral index, shape, and flux). The excellent sensitivity of XRT will enable us to fully characterize the SED from 0.3 keV - 200 MeV. Together with the simultaneous optical/UV coverage of UVOT, composing a broadband SED of these objects will enable us to (i) determine the nature of these newly discovered sources; (ii) perform a detailed study of their SED and compute their energetics.
2225162 / KAPLAN / UNIVERSITY OF WISCONSIN-MILWAUKEE
"SEARCHING FOR X-RAY EMISSION FROM NEW MAGNETIC TRANSIENTS DISCOVERED BY ASKAP/VAST"
The latest generation of widefield radio imaging surveys have begun to discover perplexing new sources, which emit bright polarized bursts that resemble those from pulsars and fast radio bursts but which last hundreds of times longer. Some are periodic on timescales of minutes to hours, and are broadly known as Long-Period Transients (LPTs). Others are totally unclassified. Their origin is unknown: they may be related to old magnetars, magnetized white dwarfs, or some other source type. What is clear is that the number of sources and their diversity in properties are both increasing. We request Swift TOO observations of 4 new transients discovered with the ASKAP/VAST survey.
2225165 / VIELIUTE / UNIVERSITY OF ST. ANDREWS
"EXTENDING SCALING RELATIONS OF THE AGN ACCRETION FLOW INTO THE LOW-MASS REGIME"
Intensive multi-wavelength monitoring experiments of AGN have provided a comprehensive view of their inner-most structure, yet there remains no robust constraint on AGN accretion flow properties in the low-mass regime. This experiment will extend the scaling relations of the AGN accretion flow down to Mbh = 10^5.5Msolar, with POX52 offering a better-constrained Mbh than the only other intensively studied low-mass AGN NGC4395. We propose to obtain Swift UV/X-Ray coverage of POX52 to extend an approved ground-based intensive monitoring experiment with ULTRACAM on the 3.6m NTT. The contemporaneous Swift and ground-based observations will provide two independent tests for the AGN accretion flow structure via the variable SED and inter-band lags.
2225166 / SAIKIA / YALE UNIVERSITY
"A SWIFT LEGACY SURVEY OF XRBS IN OUTBURST: TRACKING ACCRETION IN ACTION"
Swift has provided unparalleled X-ray and UV coverage of LMXB outbursts, capturing rises, peaks, decays, and rebrightenings over nearly two decades. We propose a legacy survey to uniformly reduce and analyze all Swift/XRT and UVOT data for outbursts of 26 LMXBs with complementary optical/IR monitoring. For each snapshot, we will extract light curves, spectra, power spectra, and hardness intensity diagrams, and integrate them with ground-based data into a quasi-simultaneous multi-wavelength archive. This public database will enable population-level studies of outburst triggers, optical X-ray delays, rebrightenings, failed transitions, absorption dips, and jet disc coupling, securing Swift s legacy in tracking accretion in action.
2225171 / BODEWITS / AUBURN UNIVERSITY
"SWIFT/UVOT AND THE WATER CYCLE OF OORT CLOUD COMETS"
We will use the Swift Ultraviolet/Optical Telescope to complete post-perihelion monitoring of Oort Cloud comet C/2024 E1 and to obtain a deep ultraviolet OH map of distant comet C/2024 T5. E1 s close approach to the Sun (0.57 au) enables the first continuous ultraviolet record of how extreme solar heating alters cometary water production and nucleus erosion. T5 remains beyond 3 au, where water sublimation is inefficient; mapping its OH coma tests whether icy grains drive the pale blue spot seen in other distant comets. Together, these targets provide a natural experiment linking volatile release and cometary evolution from the cold outer solar system to intense near-Sun heating.
2225173 / BUSON / UNIVERSITY OF WUERZBURG
"BREAKING THE DEGENERACY WITH THE NEIL GEHRELS SWIFT OBSERVATORY AND NUSTAR"
The bright gamma-ray blazar 5BZB J0630-2406 has recently been proposed as a promising neutrino emitter. Previous joint simultaneous observations revealed a break in the X-ray spectrum that challenges purely leptonic models, showing a preference for a hadronic contribution in its spectral energy distribution (SED). Lepto-hadronic models naturally explain the break observed in the X-ray data as the contribution of the hadronic component, suggesting that the hadronic imprint may have been observed. They adequately describe the SED and predict a neutrino flux at the reach of the IceCube observatory. The proposed joint Swift/NuSTAR observations aim to investigate the origin of the X-ray emission in 5BZB J0630-2406, shedding light on its potential role as a neutrino point-source.
2225175 / DELAUNAY / THE PENNSYLVANIA STATE UNIVERSITY
"DETECTING WITH SWIFT THE AFTERGLOW OF GRBS LOCALIZED BY THE NITRATES PIPELINE"
The GUANO and NITRATES pipelines have enabled a systematic search for subthreshold gamma-ray events using Swift-BAT, targeted on external triggers. In this proposal, we aim to follow up on GRBs identified by NITRATES within the BAT field of view, performing a tiling with XRT on the areas of the localization map with highest probability. Our targets include externally triggered GRBs and GWs. Detecting the afterglow with XRT will allow for precise localization of the burst, facilitating the identification of the host galaxy and determination of its redshift. This program enhances our chances of detecting faint GRBs and their afterglows, and for a GRB counterpart to a GW event the precise localization provided by NITRATES will have striking impact for multi-messenger science goals.
2225180 / MASTERSON / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"THE QPO-CORONA CONNECTION IN THE ENIGMATIC AGN 1ES 1927+654"
1ES 1927+654 defies what we thought possible for accretion onto black holes. In 2018, the source began a major outburst, becoming the first changing-look AGN caught in real time. 1ES 1927+654 exhibited extreme X-ray spectral variability during the outburst, including the destruction of the X-ray corona. Despite rebuilding its corona and returning to its pre-outburst X-ray state by 2021, this unique AGN began showing a rapidly-evolving mHz X-ray QPO and recently launched a radio jet. We propose a one year monitoring campaign with roughly one 1 ks Swift observation per week (totaling 52 ks) to track the long-term evolution of the X-ray and UV flux, connect the new mHz QPO to the evolution of the X-ray corona, and search for sudden outbursts in this legacy target.
2225181 / MILLER / TEXAS A&M UNIVERSITY
"REVERBERATION MAPPING OF CHANGING-LOOK ACTIVE GALACTIC NUCLEUS NGC5273"
We propose high-cadence X-ray and ultraviolet observations of the changing-look active galactic nucleus (AGN) NGC5273. This campaign will coincide with guaranteed optical imaging and spectroscopy from multiple ground-based robotic observatories and proposed radio monitoring. The methods and observational goals of our program can be fully executed regardless of the spectral type NGC5273 is in during the observations. The analysis presented would be the highest cadence reverberation mapping campaign of a changing-look AGN to date with complete wavelength coverage from X-ray to optical. These observations will simultaneously investigate long-standing questions regarding both the nature of AGN accretion and the changing-look AGN phenomenon.
2225186 / ARCODIA / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"USING XRT TIMING DATA TO ESTIMATE THE BH MASS IN ERO-QPE5"
Quasi-periodic eruptions (QPEs) are repeated X-ray bursts from galactic nuclei, tantalizingly associated with the low-frequency GW emitting extreme mass ratio inspirals (EMRIs). The QPE=EMRI model predicts that, unavoidably, the orbit of the secondary would precess within the orbital plane due to GR Schwarzschild precession. The ratio between apsidal and orbital period only depends on the black hole mass of the primary MBH. Thus, monitoring of the QPE arrival times in regular QPE sources allows to i) confirm/rule out this prediction ii) if confirmed, measure the BH mass independently from any other current method. We will use XRT data to carry this out for the ``well-behaved" source eRO-QPE5, and the expected precision on the BH mass is 4%.
2225188 / ARCODIA / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"PROBING THE X-RAY VARIABILITY OF LOW-MASS POST-STARBURST GALAXIES WITH SWIFT-XRT"
X-ray transients like TDEs and QPEs have been found in high abundance in post-starburst low-mass galaxies. Given the lack of a systematic method for discovering QPEs, we focus on testing a new one looking among these `special' galaxies. We identify 3 galaxies that show properties consistent with those of known QPE sources. We ask for XRT follow-up to identify the possible QPEs. If successful, this pilot study will be extended to more galaxies and may provide a new way to discover QPEs.
2225190 / DELAUNAY / THE PENNSYLVANIA STATE UNIVERSITY
"INCREASING THE RATE OF WELL-LOCALIZED TRANSIENTS WITH BAT-GUANO"
The follow up of transient events is critical to understanding their nature. Swift BAT is a unique instrument which has the capability to localize high energy transients to small sky regions. This capability has only been applicable for sources that occur within the BAT FOV and trip the BAT trigger algorithm. With the GUANO system and the NITRATES pipeline, Swift is now able to significantly contribute to the localization of transients even if BAT is not triggered. Using these capabilities, BAT will localize a larger number of transients to a smaller sky region permitting large telescope facilities to conduct follow-up observations. We propose to run, monitor, and improve the GUANO/NITRATES pipelines to streamline the localization efforts that are critical to transient follow-up.
2225194 / LIN / NORTHEASTERN UNIVERSITY
"TWO UNIQUE SOURCES IN A ROW: ESO 243-49 HLX-1 AND A NEWBORN HARD TIDAL DISRUPTION EVENT"
n Neil Gehrels Swift Observatory GI Cycle 22, we request 36x1 ks snapshots (10-day cadence) to simultaneously monitor two exceptional nearby objects: a repeatedly partial tidal disruption event (TDE) by an intermediate mass black hole (IMBH) ESO 243-49 HLX-1 and a rare hard TDE in the same galaxy cluster. For HLX-1, we aim to track the evolution of outburst separation time, likely tie to an aperiodic orbital period, and to explore the system's ultimate fate, including potential donor star ejection. For the hard TDE, we seek to capture new giant, fast X-ray flares and to identify recurrent outbursts, an intriguing behavior reported among TDEs of similar spectral properties.
2225201 / QUIMBY / SAN DIEGO STATE UNIVERSITY
"UNLOCKING HIGH-REDSHIFT SUPERLUMINOUS SUPERNOVAE"
Superluminous supernovae (SLSNe) are 5 10 magnitudes brighter in the UV than ordinary supernovae, making them visible to the highest redshifts of star formation. Their high luminosities offer rare probes of chemical enrichment, star formation histories, the high-mass end of the IMF, and galaxy evolution. To use SLSNe as tracers we must better understand their UV signatures, which are critical since only rest-frame UV will be observed at high redshift. UV data also constrain their power sources and progenitor evolution. We propose Swift/UVOT observations of eight SLSNe at z<0.2, following up the four best with detailed light curves. These will establish UV templates needed to interpret distant SLSNe with Roman, JWST, and future facilities.
2225205 / SOKOLOSKI / COLUMBIA UNIVERSITY
"PRE-ERUPTION MONITORING OF T CRB"
The immediate goal of this proposal is to use UVOT, XRT and BAT monitoring of the symbiotic recurrent nova T CrB as it approaches its next eruption to determine the physical origin of pre-eruption activity, which is challenging to explain with standard nova theory. The broader goal is to determine whether: 1) low-level nuclear burning can lead to an observational precursor months to years before a nova; or 2) some previously unrecognized phenomenon both causes a precursor event and triggers a nova in T CrB. Either option would constitute a major shift in our understanding of novae. T CrB is the best target for this study, Swift is the only facility that can carry it out, and it is time sensitive. We request that regular monitoring continues through Cycle 22 or until T CrB erupts.
2225208 / ANUMARLAPUDI / UNIVERSITY OF NORTH CAROLINA
"ON THE NATURE OF EXTRAGALACTIC RADIO TRANSIENTS DISCOVERED BY ASKAP/VAST -- EXTREME NUCLEAR VARIABILITY?"
All sky radio surveys are starting to discover highly variable extragalactic radio transients. This radio variability can not be easily explained by the AGN variability or propagation effects, indicating that these might represent explosive transients like tidal disruption events (TDEs). However, understanding the nature of these transients requires follow-up X-ray observations, as TDEs often show late-time X-ray and radio activity (correlated in a few cases), which can be used to characterize these radio sources. Understanding these radio sources (with no optical counterparts) will have a huge implication for the overall rates and opens up a new (radio) discovery avenue. Here, we propose Swift observations for 10 highly variable radio sources to understand their late-time X-ray behavior.
2225216 / STEIN / UNIVERSITY OF MARYLAND (COLLEGE PARK)
"HIGH-REDSHIFT TDES FROM RUBIN TO ROMAN"
TDEs are unique probes of SMBH demographics. With the imminent Rubin and Roman surveys, we will be able to study TDEs at high redshift (z>0.5) for the first time. TDEs are uniquely UV-bright, and can be classified efficiently with a single Swift-UVOT snapshot. We seek to classify 100 candidate high-redshift TDEs selected by Rubin, yielding the first TDE sample to study the black hole mass function at high redshift.
2225238 / FOLEY / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)
"REDUCING TYPE IA SUPERNOVA DISTANCE BIASES BY SEPARATING REDDENING AND INTRINSIC COLOR"
Accurate distance measurements and unbiased cosmological constraints from Type Ia supernovae (SNe Ia) rely on proper correction for line-of-sight host galaxy dust reddening. The current standard for measuring SN distances confounds dust reddening and the intrinsic color-luminosity correlation into a single SN color law, introducing a bias that is currently SN cosmology s most challenging systematic uncertainty. A 135-orbit Cycle 30 and 31 HST program obtained late-time UV and NIR imaging of 96 SNe Ia to break the degeneracy. Of these, 39 were observed by Swift. We propose to obtain template images for the Swift sample. We will then transfer the knowledge from the HST program to all SNe with rest-frame UV data near peak, including the full Swift sample and high-z targets from Rubin/Roman.
2225241 / WALTON / UNIVERSITY OF HERTFORDSHIRE
"A TALE OF TWO PHASES? CONTINUED MONITORING OF NGC2283 ULX1"
Following a series of remarkable discoveries, we now know that some of the most luminous members of the ultraluminous X-ray source (ULX) population are actually powered by highly super-Eddington neutron stars. However, much remains poorly understood about these enigmatic systems, in part because only 7 confirmed ULX pulsars that show sustained super-Eddington accretion are known. NGC2283 ULX1 has recently been found to exhibit a high-amplitude X-ray period with a ~40d timescale, which shows properties remarkably similar to the super-orbital X-ray periods seen from known ULX pulsars. Surprisingly, the phase solution for shows tentative evidence for being bi-modal. We therefore propose a further monitoring program with Swift (40x3ks) to test this scenario further.
2225243 / TROJA / UNIVERSITA' DEGLI STUDI DI ROMA TOR VERGATA
"A SWIFT LOOK AT SUPERNOVA SHOCK BREAK-OUTS"
Swift is an extraordinary supernova (SN) observatory. One of its unique strengths is obtaining early UV and X-ray data of young SNe, enabling robust constraints on their progenitor systems and surrounding environment. Despite the great progress of the last few years, the average delay time between the SN explosion and the start of Swift observations is around 2 days. We propose to further shrink this temporal gap by using SN shock break-out (SBO) flares discovered by the Einstein Probe telescope. The synergy between these two observatories will open a new window into the evolution of infant SNe and greatly advance our understanding of their explosion mechanisms.
2225244 / DESAI / INSTITUTE OF SCIENCE AND TECHNOLOGY AUSTRIA
"REDRAWING THE HR DIAGRAM FOR MAGNETIC WHITE DWARFS"
We propose a UV photometric census of magnetic white dwarfs (MWDs) with Swift/UVOT. We will measure the UV spectral energy distribution (SED) across the critical 1900 3000 AA window, where strong fields create a spectral break near 3000 AA, for 51 isolated MWDs that span a broad range of magnetic field strengths(0.3-1000 MG), temperatures(10-50 kK) and masses (including ultramassive MWDs). By combining UV with optical data and modelling it with new, state-of-the-art magnetic atmosphere models, we will obtain significantly improved effective temperatures and radii, enabling robust mass estimates and population-level tests of magnetic field origin scenarios. Additionally, we will be able to constrain the X-ray emission of most MWDs, exploring the extent of the newly discovered class of MWDs.
2225249 / LUNDY / COLUMBIA UNIVERSITY
"ENERGETIC EXTREMA IN 4C+42.22: CHARACTERIZING THE MOST EXTREME HIGH SYNCHROTRON PEAKED BL LACS WITH SWIFT-XRT"
Extreme high synchrotron peaked BL Lacs (eHBLs) are an exciting rare class of active galactic nuclei (AGN) that provide the ideal astrophysical laboratory for testing models of particle accelerations in jets, and of cosmology. These energetic sources are characterized by synchrotron emission peaking above 1 keV, or Compton emission peaking above 2 TeV. As the sample of known sources is approximately 20, expanding and studying the multi-wavelength properties of new members of the population is a priority. Recent observations by LHAASO have revealed a new candidate, 4C +42.22, that remains understudied in the X-ray regime. We propose targeting 4C +42.22 with Swift-XRT to measure the X-ray properties of this source in detail for the first time, potentially identifying a new eHBL.
2225250 / DURBAK / UNIVERSITY OF MARYLAND (COLLEGE PARK)
"RIMAS - RAPID INFRARED IMAGER-SPECTROMETER: A RECENTLY COMMISSIONED FACILITY FOR FAST FOLLOW-UP OF HIGH-Z GRBS"
RIMAS is a new NIR instrument designed expressly to identify high-redshift GRBs from Swift, installed on the 4.3 m Lowell Discovery Telescope (LDT) in June 2025. RIMAS can operate in and switch rapidly (10s of seconds) between four modes: 1) simultaneous 2-band imaging; 2) high-throughput, R~25; 3) R~300 NIR spectroscopy; 4) high-resolution (R~4500), cross-dispersed echelle spectroscopy providing simultaneous coverage from 0.9-2.4 um. Unlike most classically scheduled facilities, RIMAS will be continuously available for rapid-response (~3 minutes) ToO observations. By the completion of Cycle 22, RIMAS will be routinely obtaining rapid multi-color photometry and NIR spectra of Swift afterglows to measure their redshifts and constrain properties of their host galaxies and the surrounding IGM
2225252 / CLARK / SPACE TELESCOPE SCIENCE INSTITUTE
"COMBINING SWIFT & JWST TO BENCHMARK THE INTERPLAY BETWEEN RADIATION AND THE ISM, ACROSS 1 DEX IN METALLICITY"
We propose using Swift-UVOT and JWST in concert, to understand the relationship between Polycyclic Aromatic Hydrocarbons (PAHs, the smallest dust particles) and the UV radiation field in galaxy M101. The UV powers PAH emission (which dominates the mid-IR), but also processes & destroys PAHs. PAH abundance is also hugely metallicity-dependent. JWST recently targeted PAH emission in 6 fields in M101 spanning 0.93 dex in metallicity. UVOT is uniquely able to constrain hardness & intensity of the UV radiation, vital for understanding PAHs. Deep archival UVOT data covers much of M101. However the lowest-metallicity JWST region, vital for constraining relations, has no UVOT coverage. PLus lack of UVOT coverage around M101 causes background artefacts. Our new data will fix address both issues.
2225255 / BROWN / TEXAS A&M UNIVERSITY
"IMPROVING SMEARED SWIFT SUPERNOVAE WITH TEMPLATE OBSERVATIONS"
The Swift Ultra-Violet/Optical Telescope (UVOT) has revolutionized the understanding of supernova (SN) behavior in the UV. UVOT has observed over 1400 SNe, including examples of all major classes and most subtypes. This has enabled detailed studies of individual objects and to discover differences within SN subgroups. These and future studies rely on having the best possible photometric precision. Much of the original SN photometry is contaminated by the underlying host galaxy light. Additionally, the smearing of UVOT images during parts of 2023-2024 requires post-gyro observations to reliably calibrate field stars and correct the photometry. We propose reobserving the host galaxies of 46 Swift supernovae to improve the accuracy and usefulness of the SN photometry.
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