Swift Cycle 21 Results
The lists below contain the proposals recommended by the Cycle 21 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 21 proposals for observation: Please note that the ROSES 2024 Appendix D.5 "Swift Guest Investigator Cycle 21" states:
"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 21 ToO proposals may be triggered until March 31, 2026."
- 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, 2025.
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Recommended Proposals
Prop PI Title
2124005 LAHA CAUGHT IN THE ACT: A SWIFT TOO CAMPAIGN ON CHANGING-LOOK AGN
2124009 GRUPE UNDERSTANDING AGN VARIABILITY WITH RESPECT TO AGN PROPERTIES
2124011 PERNA CALIBRATING THE STELLAR POPULATION IN THE DISKS OF ACTIVE GALACTIC NUCLEI VIA GRB OBSERVATIONS
2124014 PASHAM SWIFT+NICER OBSERVATIONS TO IDENTIFY AND STUDY COSMOLOGICAL BLACK HOLES TURNING ON
RELATIVISTIC JETS
2124018 KENNEA SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS IN CYCLE 21
2124035 TOIVONEN THE LOW-LATENCY GRAVITATIONAL-WAVE ALERT SYSTEM ENABLING SWIFT FOLLOW-UP
2124040 WALTON TESTING THE LENSE-THIRRING MODEL FOR ULX VARIABILITY WITH NGC5907 ULX1
2124048 AJELLO SWIFT TOOS FOR FERMI GALACTIC PLANE TRANSIENTS
2124051 HOMAN OBSERVING THE EARLY RISE OF X-RAY TRANSIENTS WITH SWIFT
2124054 CHAKRABORTY UNDERSTANDING THE DIVERSITY OF UNEXPECTED LATE-TIME BEHAVIOR IN TIDAL DISRUPTION EVENTS
2124058 WANG PROBING THE X-RAY REPROCESSING LAG OF A PROTOTYPE INTERMEDIATE-MASS BLACK HOLE IN POX 52
2124061 VAN DEN EIJNDEN SWIFT/VLA MONITORING OF THE DECAY OF A GIANT BE/X-RAY BINARY OUTBURST
2124062 PENIL SWIFT MONITORING OF PG 1553+113, A PERIODICALLY EMITTING BLAZAR
2124064 NUNEZ COMPLETING THE X-RAY CENSUS OF GROUP-X, A NEW LABORATORY FOR INVESTIGATING THE
ACTIVITY-ROTATION RELATION
2124068 KENNEA KEY PROJECT: THE DETECTION AND MONITORING OF ELECTROMAGNETIC COUNTERPARTS OF GRAVITATIONAL
WAVE SOURCES WITH SWIFT IN O4
2124072 WOODWARD THE BRIGHTEST NOVA IN THE LAST 80 YEARS: T CORONAE BOREALIS
2124077 EDELSON INTENSIVE BROADBAND REVERBERATION MAPPING OF NGC 4151
2124078 KENNEA IDENTIFYING THE ELECTROMAGNETIC COUNTERPARTS TO COSMIC NEUTRINO SOURCES
2124087 DEGENAAR THE NATURE AND ACCRETION FLOW PROPERTIES OF SUB-LUMINOUS X-RAY BINARIES
2124095 MARGUTTI A PANCHROMATIC INVESTIGATION OF SUPER-LUMINOUS SUPERNOVAE
2124097 MARGUTTI CONSTRAINING THE NATURE OF THE MOST EXTREME EXPLOSIVE TRANSIENTS
2124101 STRADER HUNTING NEW MILLISECOND PULSAR BINARIES
2124113 AUCHETTL SWIFT'S MULTI-WAVELENGTH VIEW OF THE NEXT NEARBY TDE
2124115 BORGHESE SWIFT MONITORING OF MAGNETAR OUTBURSTS
2124119 FUERST SWIFT MONITORING OF THE ULTRA-LUMINOUS X-RAY PULSAR NGC 7793 P13
2124127 MASTERSON A LATE-TIME X-RAY VIEW OF MID-INFRARED-SELECTED TDE CANDIDATES
2124131 LANZ AGN CHARACTERISTICS OF RECENTLY QUENCHED GALAXIES
2124135 SIEGEL COMPLETING THE UV CENSUS OF GALACTIC GLOBULAR CLUSTERS
2124137 GAUDIN DEEP MONITORING OF THE SMC BE/X-RAY BINARY POPULATION DURING LUMINOUS OUTBURST
2124138 DICHIARA SEARCHING HIGH AND LOW FOR ELUSIVE SHORT GRBS
2124145 DELAUNAY INCREASING THE RATE OF WELL-LOCALIZED TRANSIENTS WITH BAT-GUANO
2124146 SOKOLOSKI MULTI-WAVELENGTH PRE-ERUPTION MONITORING OF T CRB
2124152 RAJGURU TRACING THE MOST POWERFUL JETS THROUGH COSMIC TIME
2124154 CHIRENTI A SEARCH FOR QUASIPERIODIC OSCILLATIONS IN SHORT GAMMA RAY BURSTS DETECTED BY SWIFT/BAT
2124156 BODEWITS THE ACTIVITY AND EVOLUTION OF OORT CLOUD COMETS AT A WIDE RANGE OF DISTANCES
2124165 MARCULEWICZ WEAK EMISSION-LINE QUASARS IN THE UV - THE MISSING PIECE TO CONSTRAIN THE BLACK HOLE MASS
2124177 VIELIUTE DISENTANGLING THE SPECTRAL ENERGY DISTRIBUTION OF AGN IN INTENSIVE GROUND-BASED
MONITORING CAMPAIGNS
2124184 KAPLAN SEARCHING FOR X-RAY EMISSION FROM NEW MAGNETIC TRANSIENTS DISCOVERED BY ASKAP/VAST
2124185 MOONEY INVESTIGATING THE X-RAY AND TEV CORRELATION OF VER J0521+211 WITH SWIFT-XRT AND VERITAS
2124187 SAND UV IMAGING OF NEWLY DISCOVERED DWARF GALAXIES IN THE VERY NEARBY UNIVERSE
2124192 LINCETTO SWIFT FOLLOW UP OF KM3NET HIGH-ENERGY NEUTRINO EVENTS
2124198 MCBRIDE X-RAY SIGNATURES OF NEUTRINO EMITTERS
2124203 CLARK COMBINING SWIFT & JWST TO BENCHMARK THE INTERPLAY BETWEEN RADIATION AND THE ISM, ACROSS
1 DEX IN METALLICITY
2124205 HOSSEINZADEH ULTRA-RAPID, HIGH-CADENCE UV PHOTOMETRY OF INFANT SUPERNOVAE
2124207 HAMMERSTEIN STELLAR DESTRUCTION ON THE RISE: INFANT TIDAL DISRUPTION EVENTS WITH SWIFT
2124211 LIN TWO UNIQUE SOURCES IN A ROW: ESO 243-49 HLX-1 AND A NEWBORN HARD TIDAL DISRUPTION EVENT
2124212 LAWTHER CAPTURING THE BRIGHT STATE OF A RE-IGNITED AGN
2124218 WALSH SWIFT AND THE VLBA UNMASK THE CHANGING-LOOK AGN MRK 590
2124237 SANTANDER PINPOINTING THE SOURCES OF THE ISOTROPIC GAMMA-RAY BACKGROUND WITH SWIFT
2124240 WARD EXPLORING THE PHYSICAL ORIGIN OF COMPACT MILLIMETER EMISSION IN RADIO-QUIET AGN WITH
SWIFT X-RAY MONITORING
2124242 DURBAK RIMAS - RAPID INFRARED IMAGER-SPECTROMETER A FACILITY FOR A FAST FOLLOWUP ON HIGH REDSHIFT GRBS
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] | 2124005 | LAHA | 1 | TOO CL-AGN | 96 | Y | 0 | 0 | 2124009 | GRUPE | 1 | RX J0022.5-3407 | 1 | N | 5.63917 | -34.12222 | 2124009 | GRUPE | 2 | ESO 242-G8 | 1 | N | 6.25083 | -45.49278 | 2124009 | GRUPE | 3 | TON S 180 | 1 | N | 14.33417 | -22.3825 | 2124009 | GRUPE | 4 | QSO 0056-36 | 1 | N | 14.65583 | -36.10139 | 2124009 | GRUPE | 5 | RX J0100-5113 | 1 | N | 15.11292 | -51.23167 | 2124009 | GRUPE | 6 | RX J0105.6-141 | 1 | N | 16.41167 | -14.27056 | 2124009 | GRUPE | 7 | RX J0117-3826 | 1 | N | 19.3775 | -38.44167 | 2124009 | GRUPE | 8 | MS 0117-28 | 1 | N | 19.89875 | -28.35889 | 2124009 | GRUPE | 9 | RX J0128.1-1848 | 1 | N | 22.02792 | -18.80861 | 2124009 | GRUPE | 10 | IRAS F01267-217 | 1 | N | 22.29458 | -21.69917 | 2124009 | GRUPE | 11 | RX J0134.2-4258 | 1.4 | N | 23.57042 | -42.97417 | 2124009 | GRUPE | 12 | RX J0136.9-3510 | 1.25 | N | 24.22667 | -35.16444 | 2124009 | GRUPE | 13 | RX J0148.3-2758 | 1 | N | 27.09292 | -27.97389 | 2124009 | GRUPE | 14 | RX J0152.4-2319 | 1 | N | 28.11292 | -23.33167 | 2124009 | GRUPE | 15 | MKN 1044 | 1 | N | 37.52292 | -8.99806 | 2124009 | GRUPE | 16 | MKN 1048 | 1 | N | 38.6575 | -8.78778 | 2124009 | GRUPE | 17 | RX J0311.3-2046 | 1 | N | 47.82833 | -20.77194 | 2124009 | GRUPE | 18 | RX J0319.8-2627 | 1 | N | 49.95292 | -26.45333 | 2124009 | GRUPE | 19 | RX J0323.2-4931 | 1.4 | N | 50.81583 | -49.51972 | 2124009 | GRUPE | 20 | ESO 301-G13 | 1 | N | 51.26042 | -41.905 | 2124009 | GRUPE | 21 | VCV 0331-37 | 1 | N | 53.4175 | -37.11528 | 2124009 | GRUPE | 22 | RX J0349.1-4711 | 1.7 | N | 57.28208 | -47.18444 | 2124009 | GRUPE | 23 | FAIRALL 1116 | 1 | N | 57.92375 | -40.46667 | 2124009 | GRUPE | 24 | FAIRALL 1119 | 1 | N | 61.25708 | -37.1875 | 2124009 | GRUPE | 25 | RX J0412.7-4712 | 1 | N | 63.17292 | -47.21278 | 2124009 | GRUPE | 26 | 1H 0419-577 | 1 | N | 66.50292 | -57.20056 | 2124009 | GRUPE | 27 | FAIRALL 303 | 1 | N | 67.66667 | -53.61556 | 2124009 | GRUPE | 28 | RX J0435.2-4615 | 1 | N | 68.81 | -46.25917 | 2124009 | GRUPE | 29 | RX J0435.9-3636 | 1 | N | 68.97458 | -36.61139 | 2124009 | GRUPE | 30 | RX J0437.4-4711 | 1 | N | 69.3675 | -47.19167 | 2124009 | GRUPE | 31 | RX J0439.6-5311 | 1 | N | 69.91125 | -53.19194 | 2124009 | GRUPE | 32 | 1H 0439-272 | 1 | N | 70.34375 | -27.13889 | 2124009 | GRUPE | 33 | RX J0454.7-4813 | 1 | N | 73.67917 | -48.22222 | 2124009 | GRUPE | 34 | PKS 0558-504 | 1 | N | 89.9475 | -50.44778 | 2124009 | GRUPE | 35 | 1 ES 0614-584 | 1 | N | 93.95667 | -58.435 | 2124009 | GRUPE | 36 | RX J0859.0+4846 | 1 | N | 134.76208 | 48.76917 | 2124009 | GRUPE | 37 | RX J0902.5-0700 | 1.7 | N | 135.64 | -7.00111 | 2124009 | GRUPE | 38 | MKN 110 | 1 | N | 141.30417 | 52.28667 | 2124009 | GRUPE | 39 | PMN J0948+00222 | 1.4 | N | 147.2375 | 0.37361 | 2124009 | GRUPE | 40 | PG 0953+414 | 1 | N | 149.21833 | 41.25611 | 2124009 | GRUPE | 41 | RX J0435.2-4615 | 1 | N | 68.81 | -46.25917 | 2124009 | GRUPE | 42 | RX J1005.7+4332 | 1.25 | N | 151.42458 | 43.54472 | 2124009 | GRUPE | 43 | RX J1007.1+2203 | 1.4 | N | 151.7925 | 22.05056 | 2124009 | GRUPE | 44 | CBS 126 | 1 | N | 153.2625 | 35.85667 | 2124009 | GRUPE | 45 | RX J1017.3+2914 | 1 | N | 154.32625 | 29.24278 | 2124009 | GRUPE | 46 | HS 1019+37 | 1.25 | N | 154.75208 | 37.87806 | 2124009 | GRUPE | 47 | MKN 141 | 2 | N | 154.8025 | 63.9675 | 2124009 | GRUPE | 48 | MKN 142 | 1 | N | 156.38042 | 51.67639 | 2124009 | GRUPE | 49 | RX J1034.6+3938 | 1 | N | 158.66083 | 39.64111 | 2124009 | GRUPE | 50 | EXO 1055+60 | 1 | N | 164.62542 | 60.26694 | 2124009 | GRUPE | 51 | RX J1117.1+6522 | 1 | N | 169.29208 | 65.36861 | 2124009 | GRUPE | 52 | PG 1115+407 | 1 | N | 169.62667 | 40.43194 | 2124009 | GRUPE | 53 | TON 1388 | 1 | N | 169.78625 | 21.32167 | 2124009 | GRUPE | 54 | EXO 1128+69 | 1 | N | 172.77 | 68.86472 | 2124009 | GRUPE | 55 | 2B 1128+31 | 1 | N | 172.78958 | 31.235 | 2124009 | GRUPE | 56 | SBS 1136+579 | 1.25 | N | 174.70667 | 57.71222 | 2124009 | GRUPE | 57 | Z 1136+3412 | 1 | N | 174.80792 | 33.93083 | 2124009 | GRUPE | 58 | WAS 26 | 1 | N | 175.3175 | 21.93917 | 2124009 | GRUPE | 59 | CASG 855 | 2 | N | 176.12458 | 36.88583 | 2124009 | GRUPE | 60 | CSO 109 | 1 | N | 176.29292 | 30.78806 | 2124009 | GRUPE | 61 | MKN 1310 | 1 | N | 180.31 | -3.67806 | 2124009 | GRUPE | 62 | NGC 4051 | 1 | N | 180.78958 | 44.53056 | 2124009 | GRUPE | 63 | GQ COMAE | 1 | N | 181.17542 | 27.90333 | 2124009 | GRUPE | 64 | RX J1209.8+3217 | 2 | N | 182.43833 | 32.28389 | 2124009 | GRUPE | 65 | PG 1211+143 | 1 | N | 183.57375 | 14.05361 | 2124009 | GRUPE | 66 | MKN 766 | 1 | N | 184.61083 | 29.81278 | 2124009 | GRUPE | 67 | RX J1231.6+7044 | 1 | N | 187.9025 | 70.73722 | 2124009 | GRUPE | 68 | MKN 771 | 1 | N | 188.015 | 20.15833 | 2124009 | GRUPE | 69 | TON 83 | 1.4 | N | 188.42375 | 31.0175 | 2124009 | GRUPE | 70 | MCG+08-23-067 | 1.7 | N | 189.21333 | 45.65139 | 2124009 | GRUPE | 71 | NGC 4593 | 1 | N | 189.91417 | -5.34417 | 2124009 | GRUPE | 72 | IRAS F12397+3333 | 1 | N | 190.54417 | 33.28417 | 2124009 | GRUPE | 73 | PG 1244+026 | 1 | N | 191.64667 | 2.36917 | 2124009 | GRUPE | 74 | RX J1304.2+0205 | 2 | N | 196.07083 | 2.09361 | 2124009 | GRUPE | 75 | PG 1307+085 | 2 | N | 197.44583 | 8.33 | 2124009 | GRUPE | 76 | RX J1312.9+2628 | 2 | N | 198.24792 | 26.47417 | 2124009 | GRUPE | 77 | RX J1314.3+3429 | 2 | N | 198.59458 | 34.49417 | 2124009 | GRUPE | 78 | RX J1319.9+5235 | 1 | N | 199.98792 | 52.5925 | 2124009 | GRUPE | 79 | PG 1322+659 | 1.4 | N | 200.95625 | 65.69667 | 2124009 | GRUPE | 80 | IRAS 13349+2438 | 1 | N | 204.32792 | 24.38417 | 2124009 | GRUPE | 81 | TON 730 | 1 | N | 205.98625 | 25.64667 | 2124009 | GRUPE | 82 | 2E 13 46+2637 | 2 | N | 207.14292 | 26.36861 | 2124009 | GRUPE | 83 | RX J1355.2+5612 | 1 | N | 208.81917 | 56.2125 | 2124009 | GRUPE | 84 | PG 1402+261 | 1 | N | 211.3175 | 25.92611 | 2124009 | GRUPE | 85 | RX J1413.6+7029 | 1 | N | 213.40292 | 70.49722 | 2124009 | GRUPE | 86 | QSO 1421-0013 | 1 | N | 216.01583 | -0.44944 | 2124009 | GRUPE | 87 | MKN 813 | 1 | N | 216.85417 | 19.83139 | 2124009 | GRUPE | 88 | MKN 684 | 1 | N | 217.76708 | 28.28722 | 2124009 | GRUPE | 89 | MKN 478 | 1 | N | 220.53125 | 35.43972 | 2124009 | GRUPE | 90 | PG 1448+273 | 1 | N | 222.78667 | 27.1575 | 2124009 | GRUPE | 91 | MKN 841 | 1 | N | 226.005 | 10.43778 | 2124009 | GRUPE | 92 | SBS 1517+520 | 2 | N | 229.63667 | 51.91583 | 2124009 | GRUPE | 93 | SBS 1527+564 | 1 | N | 232.28125 | 56.26861 | 2124009 | GRUPE | 94 | MKN 493 | 2 | N | 239.79042 | 35.03 | 2124009 | GRUPE | 95 | MKN 876 | 1 | N | 243.48833 | 65.71972 | 2124009 | GRUPE | 96 | RX J1618.1+3619 | 1 | N | 244.53917 | 36.33278 | 2124009 | GRUPE | 97 | KUG 1618+40 | 2 | N | 244.96375 | 40.98 | 2124009 | GRUPE | 98 | PG 1626+554 | 1 | N | 246.98375 | 55.37556 | 2124009 | GRUPE | 99 | EXO 1627+4014 | 1.7 | N | 247.25542 | 40.13333 | 2124009 | GRUPE | 100 | RX J1646.4+3929 | 1 | N | 251.60833 | 39.4925 | 2124009 | GRUPE | 101 | RX J1702.5+3247 | 1 | N | 255.62958 | 32.78889 | 2124009 | GRUPE | 102 | PKS 2004-447 | 2 | N | 301.98 | -44.57889 | 2124009 | GRUPE | 103 | II ZW 136 | 1 | N | 323.11625 | 10.13889 | 2124009 | GRUPE | 104 | RX J2146.6-3051 | 1 | N | 326.65 | -30.86139 | 2124009 | GRUPE | 105 | RX J2154.8-4414 | 1 | N | 328.71333 | -44.235 | 2124009 | GRUPE | 106 | ESO 404-G029 | 1 | N | 331.9375 | -32.58361 | 2124009 | GRUPE | 107 | NGC 7214 | 1 | N | 332.27917 | -27.81 | 2124009 | GRUPE | 108 | RX J2213.0-1710 | 1 | N | 333.25125 | -17.17167 | 2124009 | GRUPE | 109 | RX J2216.8-4451 | 1 | N | 334.22167 | -44.86583 | 2124009 | GRUPE | 110 | RX J2217.9-5941 | 3 | N | 334.48583 | -59.69167 | 2124009 | GRUPE | 111 | PKS 2227-399 | 1 | N | 337.66792 | -39.71444 | 2124009 | GRUPE | 112 | RX J2241.9-4404 | 2 | N | 340.48167 | -44.08194 | 2124009 | GRUPE | 113 | RX J2242.6-3845 | 1.25 | N | 340.65708 | -38.75444 | 2124009 | GRUPE | 114 | RX J2245.2-4652 | 1.7 | N | 341.33458 | -46.87 | 2124009 | GRUPE | 115 | MS 2254-36 | 1 | N | 344.4125 | -36.93528 | 2124009 | GRUPE | 116 | RX J2258.7-2609 | 1 | N | 344.68917 | -26.15389 | 2124009 | GRUPE | 117 | RX J2301.6-5913 | 1 | N | 345.40083 | -59.22222 | 2124009 | GRUPE | 118 | RX J2301.8-5508 | 1.25 | N | 345.46667 | -55.14194 | 2124009 | GRUPE | 119 | RX J2303.9-5517 | 1 | N | 345.99167 | -55.28833 | 2124009 | GRUPE | 120 | RX J2304.6-3501 | 2 | N | 346.15542 | -35.02028 | 2124009 | GRUPE | 121 | RX J2312.5-3404 | 1.25 | N | 348.145 | -34.07222 | 2124009 | GRUPE | 122 | RX J2314.9+2243 | 2 | N | 348.73208 | 22.72278 | 2124009 | GRUPE | 123 | RX J2317.8-4422 | 2 | N | 349.45792 | -44.37444 | 2124009 | GRUPE | 124 | RX J2325.2-3236 | 1 | N | 351.29917 | -32.60972 | 2124009 | GRUPE | 125 | IRAS F23226-3843 | 2 | N | 351.35083 | -38.44694 | 2124009 | GRUPE | 126 | MS 23409-1511 | 1 | N | 355.86917 | -14.925 | 2124009 | GRUPE | 127 | RX J2349.4-3126 | 2 | N | 357.35042 | -31.43417 | 2124009 | GRUPE | 128 | AM 2354-304 | 1 | N | 359.36667 | -30.46111 | 2124014 | PASHAM | 1 | RELATIVISTIC_TDE | 40 | Y | 0 | 0 | 2124018 | KENNEA | 1 | MAXI TRANSIENT #1 | 1 | Y | 0 | 0 | 2124018 | KENNEA | 2 | MAXI TRANSIENT #2 | 1 | Y | 0 | 0 | 2124018 | KENNEA | 3 | MAXI TRANSIENT #3 | 1 | Y | 0 | 0 | 2124018 | KENNEA | 4 | MAXI TRANSIENT #4 | 2 | Y | 0 | 0 | 2124018 | KENNEA | 5 | MAXI TRANSIENT #5 | 2 | Y | 0 | 0 | 2124018 | KENNEA | 6 | MAXI TRANSIENT #6 | 3.5 | Y | 0 | 0 | 2124040 | WALTON | 1 | NGC5907 ULX1 | 104 | N | 228.99571 | 56.30303 | 2124048 | AJELLO | 1 | FAVA_TARGET1 | 15 | Y | 0 | 0 | 2124048 | AJELLO | 2 | FAVA_TARGET2 | 15 | Y | 0 | 0 | 2124051 | HOMAN | 1 | TRANSIENT 1 | 20 | Y | 0 | 0 | 2124051 | HOMAN | 2 | TRANSIENT 2 | 20 | Y | 0 | 0 | 2124054 | CHAKRABORTY | 1 | AT2019AZH | 2 | N | 123.32058 | 22.64831 | 2124054 | CHAKRABORTY | 2 | AT2022DBL | 2 | N | 185.18779 | 49.55128 | 2124054 | CHAKRABORTY | 3 | AT2018ZR | 2 | N | 119.22729 | 34.26211 | 2124054 | CHAKRABORTY | 4 | AT2018BSI | 2 | N | 123.86092 | 45.59219 | 2124054 | CHAKRABORTY | 5 | AT2018HCO | 2 | N | 16.89012 | 23.47617 | 2124054 | CHAKRABORTY | 6 | AT2018IIH | 2 | N | 262.01629 | 30.69206 | 2124054 | CHAKRABORTY | 7 | AT2018HYZ | 2 | N | 151.712 | 1.69278 | 2124054 | CHAKRABORTY | 8 | AT2018LNA | 2 | N | 105.82771 | 23.02908 | 2124054 | CHAKRABORTY | 9 | AT2019BHF | 2 | N | 227.3165 | 16.23956 | 2124054 | CHAKRABORTY | 10 | AT2019DSG | 2 | N | 314.26229 | 14.2045 | 2124054 | CHAKRABORTY | 11 | AT2019EHZ | 2 | N | 212.4245 | 55.49111 | 2124054 | CHAKRABORTY | 12 | AT2019LWU | 2 | N | 347.80129 | -1.00297 | 2124054 | CHAKRABORTY | 13 | AT2019QIZ | 2 | N | 71.65783 | -10.22631 | 2124054 | CHAKRABORTY | 14 | AT2019VCB | 2 | N | 189.73479 | 33.16586 | 2124054 | CHAKRABORTY | 15 | AT2020PJ | 2 | N | 232.89571 | 33.09489 | 2124054 | CHAKRABORTY | 16 | AT2022GRI | 2 | N | 109.5865 | 33.99486 | 2124054 | CHAKRABORTY | 17 | AT2020MOT | 2 | N | 7.80625 | 85.00881 | 2124054 | CHAKRABORTY | 18 | AT2020NEH | 2 | N | 230.33371 | 14.06958 | 2124054 | CHAKRABORTY | 19 | AT2020NOV | 2 | N | 254.55408 | 2.1175 | 2124054 | CHAKRABORTY | 20 | AT2020VWL | 2 | N | 232.6575 | 26.98242 | 2124054 | CHAKRABORTY | 21 | AT2020WEY | 2 | N | 136.35779 | 61.80256 | 2124054 | CHAKRABORTY | 22 | AT2020ZSO | 2 | N | 335.57129 | -7.26636 | 2124054 | CHAKRABORTY | 23 | AT2020ACKA | 2 | N | 238.75808 | 16.30453 | 2124054 | CHAKRABORTY | 24 | AT2021AXU | 2 | N | 176.6515 | 30.08542 | 2124054 | CHAKRABORTY | 25 | AT2021EHB | 2 | N | 46.94925 | 40.31133 | 2124054 | CHAKRABORTY | 26 | AT2021JJM | 2 | N | 219.87771 | -27.8585 | 2124054 | CHAKRABORTY | 27 | AT2021MHG | 2 | N | 4.92871 | 29.31686 | 2124054 | CHAKRABORTY | 28 | AT2021NWA | 2 | N | 238.46371 | 55.58878 | 2124054 | CHAKRABORTY | 29 | AT2021SDU | 2 | N | 17.84958 | 50.57489 | 2124054 | CHAKRABORTY | 30 | AT2021YZV | 2 | N | 105.2775 | 40.82517 | 2124054 | CHAKRABORTY | 31 | AT2022AEE | 2 | N | 132.18008 | 80.88328 | 2124054 | CHAKRABORTY | 32 | AT2022RZ | 2 | N | 234.49 | 56.27161 | 2124054 | CHAKRABORTY | 33 | AT2022ADM | 2 | N | 216.96429 | 28.17478 | 2124054 | CHAKRABORTY | 34 | AT2022BDW | 2 | N | 126.29308 | 18.58264 | 2124054 | CHAKRABORTY | 35 | AT2022ARB | 2 | N | 156.043 | -0.823 | 2124054 | CHAKRABORTY | 36 | AT2022DYT | 2 | N | 150.03329 | 26.46069 | 2124054 | CHAKRABORTY | 37 | AT2022EXR | 2 | N | 262.46042 | 25.84217 | 2124054 | CHAKRABORTY | 38 | AT2022IBQ | 2 | N | 267.64908 | 21.27497 | 2124054 | CHAKRABORTY | 39 | AT2022HVP | 2 | N | 148.6885 | 55.44036 | 2124054 | CHAKRABORTY | 40 | AT2022PNA | 2 | N | 25.48142 | -3.28961 | 2124054 | CHAKRABORTY | 41 | AT2022LRI | 2 | N | 35.03338 | -22.72089 | 2124054 | CHAKRABORTY | 42 | AT2022UPJ | 2 | N | 5.98692 | -14.42319 | 2124054 | CHAKRABORTY | 43 | AT2022WTN | 2 | N | 350.84908 | 10.6855 | 2124054 | CHAKRABORTY | 44 | AT2023CVB | 2 | N | 288.607 | 41.66925 | 2124054 | CHAKRABORTY | 45 | AT2023MHS | 2 | N | 205.81529 | 19.25025 | 2124054 | CHAKRABORTY | 46 | AT2018LNI | 2 | N | 62.40688 | 73.89492 | 2124054 | CHAKRABORTY | 47 | AT2019CHO | 2 | N | 193.78837 | 49.51942 | 2124054 | CHAKRABORTY | 48 | AT2019EVE | 2 | N | 172.20687 | 15.67286 | 2124054 | CHAKRABORTY | 49 | AT2019MHA | 2 | N | 244.11583 | 56.43231 | 2124054 | CHAKRABORTY | 50 | AT2019MEG | 2 | N | 281.31742 | 44.43867 | 2124054 | CHAKRABORTY | 51 | AT2018JBV | 2 | N | 197.68983 | 8.56786 | 2124054 | CHAKRABORTY | 52 | AT2019TEQ | 2 | N | 284.77292 | 47.51825 | 2124054 | CHAKRABORTY | 53 | AT2020DDV | 2 | N | 149.63904 | 46.91119 | 2124054 | CHAKRABORTY | 54 | AT2020OPY | 2 | N | 239.10721 | 23.37253 | 2124054 | CHAKRABORTY | 55 | AT2020MBQ | 2 | N | 235.06367 | 25.00136 | 2124054 | CHAKRABORTY | 56 | AT2020QHS | 2 | N | 34.47487 | -9.61414 | 2124054 | CHAKRABORTY | 57 | AT2020RIZ | 2 | N | 32.62817 | 9.07408 | 2124054 | CHAKRABORTY | 58 | AT2020YSG | 2 | N | 171.35842 | 27.44061 | 2124054 | CHAKRABORTY | 59 | AT2019BAF | 2 | N | 268.00063 | 65.62667 | 2124054 | CHAKRABORTY | 60 | AT2019CMW | 2 | N | 282.16446 | 51.01353 | 2124054 | CHAKRABORTY | 61 | AT2020VDQ | 2 | N | 152.22267 | 42.71672 | 2124054 | CHAKRABORTY | 62 | AT2020YUE | 2 | N | 165.00137 | 21.11272 | 2124054 | CHAKRABORTY | 63 | AT2020ABRI | 2 | N | 202.322 | 19.67092 | 2124054 | CHAKRABORTY | 64 | AT2021CRK | 2 | N | 176.27896 | 18.54036 | 2124054 | CHAKRABORTY | 65 | AT2021QTH | 2 | N | 302.91221 | -21.16017 | 2124054 | CHAKRABORTY | 66 | AT2021UQV | 2 | N | 8.16617 | 22.54889 | 2124054 | CHAKRABORTY | 67 | AT2021UTQ | 2 | N | 229.62117 | 73.35872 | 2124054 | CHAKRABORTY | 68 | AT2021YTE | 2 | N | 103.76971 | 12.63417 | 2124054 | CHAKRABORTY | 69 | AT2020OCN | 2 | N | 208.47442 | 53.99733 | 2124054 | CHAKRABORTY | 70 | AT2020ADGM | 2 | N | 63.26021 | -53.07269 | 2124054 | CHAKRABORTY | 71 | AT2018DYB | 2 | N | 242.74487 | -60.92311 | 2124054 | CHAKRABORTY | 72 | AT2023CLX | 2 | N | 175.03917 | 15.32736 | 2124054 | CHAKRABORTY | 73 | AT2022DSB | 2 | N | 235.59058 | -22.67056 | 2124054 | CHAKRABORTY | 74 | AT2019AHK | 2 | N | 105.04812 | -66.04003 | 2124054 | CHAKRABORTY | 75 | AT2018FYK | 2 | N | 342.56658 | -44.86481 | 2124054 | CHAKRABORTY | 76 | AT2020KSF | 2 | N | 323.86358 | -18.27653 | 2124054 | CHAKRABORTY | 77 | AT2022GDW | 2 | N | 208.49258 | 50.04175 | 2124054 | CHAKRABORTY | 78 | AT2022FPX | 2 | N | 232.76542 | 53.40536 | 2124054 | CHAKRABORTY | 79 | AT2022CZY | 2 | N | 185.50471 | 16.99556 | 2124054 | CHAKRABORTY | 80 | AT2021UVZ | 2 | N | 263.21046 | 33.03289 | 2124054 | CHAKRABORTY | 81 | AT2021QXV | 2 | N | 229.74708 | -3.19586 | 2124054 | CHAKRABORTY | 82 | AT2021JSG | 2 | N | 167.15296 | 30.76128 | 2124054 | CHAKRABORTY | 83 | AT2021GJE | 2 | N | 252.53054 | 34.81883 | 2124054 | CHAKRABORTY | 84 | AT2021BLZ | 2 | N | 68.13021 | -32.43067 | 2124054 | CHAKRABORTY | 85 | AT2021ACK | 2 | N | 208.29162 | 9.74036 | 2124054 | CHAKRABORTY | 86 | AT2021LO | 2 | N | 46.10979 | 4.74564 | 2124054 | CHAKRABORTY | 87 | SRGE J013204.6+12223 | 2 | N | 23.01867 | 12.37656 | 2124054 | CHAKRABORTY | 88 | SRGE J021939.9+36181 | 2 | N | 34.91625 | 36.30506 | 2124054 | CHAKRABORTY | 89 | SRGE J071310.6+72562 | 2 | N | 108.29383 | 72.94075 | 2124054 | CHAKRABORTY | 90 | SRGE J091747.6+52482 | 2 | N | 139.4475 | 52.80564 | 2124054 | CHAKRABORTY | 91 | SRGE J095928.6+64302 | 2 | N | 149.86867 | 64.50606 | 2124054 | CHAKRABORTY | 92 | SRGE J133053.3+73482 | 2 | N | 202.72092 | 73.80675 | 2124054 | CHAKRABORTY | 93 | SRGE J135514.8+31160 | 2 | N | 208.81258 | 31.26811 | 2124054 | CHAKRABORTY | 94 | SRGE J144738.4+67182 | 2 | N | 221.91279 | 67.30508 | 2124054 | CHAKRABORTY | 95 | SRGE J153503.4+45505 | 2 | N | 233.76317 | 45.84861 | 2124054 | CHAKRABORTY | 96 | SRGE J161001.2+33012 | 2 | N | 242.50592 | 33.02242 | 2124054 | CHAKRABORTY | 97 | SRGE J163030.2+47012 | 2 | N | 247.62604 | 47.02372 | 2124054 | CHAKRABORTY | 98 | SRGE J163831.7+53402 | 2 | N | 249.63342 | 53.67294 | 2124054 | CHAKRABORTY | 99 | SRGE J171423.6+08523 | 2 | N | 258.59838 | 8.87692 | 2124054 | CHAKRABORTY | 100 | GSN 069 | 2 | N | 19.78333 | -34.19167 | 2124054 | CHAKRABORTY | 101 | 2XMM J123103.2+11064 | 2 | N | 187.7625 | 11.1135 | 2124054 | CHAKRABORTY | 102 | 2XMMI J184725.1-6317 | 2 | N | 281.85417 | -63.29028 | 2124054 | CHAKRABORTY | 103 | 3XMM J150052.0+01545 | 2 | N | 225.21667 | 1.91494 | 2124054 | CHAKRABORTY | 104 | 3XMM J152130.7+07491 | 2 | N | 230.37917 | 7.82125 | 2124054 | CHAKRABORTY | 105 | 3XMM J215022.4-05510 | 2 | N | 327.59167 | -5.85222 | 2124054 | CHAKRABORTY | 106 | ASASSN-14AE | 2 | N | 167.16667 | 34.09783 | 2124054 | CHAKRABORTY | 107 | ASASSN-14LI | 2 | N | 192.0625 | 17.774 | 2124054 | CHAKRABORTY | 108 | ASASSN-15LH | 2 | N | 330.5625 | -61.65972 | 2124054 | CHAKRABORTY | 109 | ASASSN-15OI | 2 | N | 309.7875 | -30.75556 | 2124054 | CHAKRABORTY | 110 | ASASSN-20IL | 2 | N | 75.79583 | -22.81444 | 2124054 | CHAKRABORTY | 111 | AT2016EZH | 2 | N | 29.52083 | 0.87278 | 2124054 | CHAKRABORTY | 112 | AT2017EQX | 2 | N | 336.7 | 17.14778 | 2124054 | CHAKRABORTY | 113 | CSS100217 | 2 | N | 157.30417 | 40.7055 | 2124054 | CHAKRABORTY | 114 | CXOU J0332 | 2 | N | 53.1625 | -27.85944 | 2124054 | CHAKRABORTY | 115 | D23H-1 | 2 | N | 353 | 0.28739 | 2124054 | CHAKRABORTY | 116 | D3-13 | 2 | N | 214.875 | 52.86844 | 2124054 | CHAKRABORTY | 117 | DES14C1KIA | 2 | N | 53.69583 | -26.32639 | 2124054 | CHAKRABORTY | 118 | DOUGIE | 2 | N | 182.2 | 43.02231 | 2124054 | CHAKRABORTY | 119 | F01004-2237 | 2 | N | 15.70833 | -22.36583 | 2124054 | CHAKRABORTY | 120 | IPTF16AXA | 2 | N | 255.89167 | 30.5935 | 2124054 | CHAKRABORTY | 121 | IPTF16FNL | 2 | N | 7.4875 | 32.89367 | 2124054 | CHAKRABORTY | 122 | J155223 | 2 | N | 238.09583 | 32.58197 | 2124054 | CHAKRABORTY | 123 | NGC 3599 | 2 | N | 168.8625 | 18.11036 | 2124054 | CHAKRABORTY | 124 | NGC 5905 | 2 | N | 228.84583 | 55.51711 | 2124054 | CHAKRABORTY | 125 | OGLE16AAA | 2 | N | 16.8375 | -64.2725 | 2124054 | CHAKRABORTY | 126 | OGLE17AAJ | 2 | N | 29.10417 | -71.07111 | 2124054 | CHAKRABORTY | 127 | PGC 1127938 | 2 | N | 19.68333 | -1.15194 | 2124054 | CHAKRABORTY | 128 | PGC 1185375 | 2 | N | 225.95833 | 1.12686 | 2124054 | CHAKRABORTY | 129 | PGC 1190358 | 2 | N | 226.37083 | 1.29256 | 2124054 | CHAKRABORTY | 130 | PGC 133344 | 2 | N | 325.73333 | -30.13278 | 2124054 | CHAKRABORTY | 131 | PGC 170392 | 2 | N | 336.69167 | -15.02306 | 2124054 | CHAKRABORTY | 132 | PS1-10ADI | 2 | N | 310.6875 | 15.50892 | 2124054 | CHAKRABORTY | 133 | PS1-10JH | 2 | N | 242.36667 | 53.67333 | 2124054 | CHAKRABORTY | 134 | PS1-11AF | 2 | N | 149.3625 | 3.23358 | 2124054 | CHAKRABORTY | 135 | PS1-13JW | 2 | N | 131.225 | 42.96244 | 2124054 | CHAKRABORTY | 136 | PTF09AXC | 2 | N | 223.30417 | 22.24231 | 2124054 | CHAKRABORTY | 137 | PTF09DJL | 2 | N | 248.48333 | 30.23794 | 2124054 | CHAKRABORTY | 138 | PTF09GE | 2 | N | 224.2625 | 49.61139 | 2124054 | CHAKRABORTY | 139 | PTF10IYA | 2 | N | 219.67083 | 37.65931 | 2124054 | CHAKRABORTY | 140 | PTF10NUJ | 2 | N | 246.60417 | 54.70594 | 2124054 | CHAKRABORTY | 141 | RX J1242-11A | 2 | N | 190.65417 | -11.32639 | 2124054 | CHAKRABORTY | 142 | RX J1420+53 | 2 | N | 215.1 | 53.56992 | 2124054 | CHAKRABORTY | 143 | SDSSJ0159 | 2 | N | 29.99167 | 0.55292 | 2124054 | CHAKRABORTY | 144 | SDSSJ0952 | 2 | N | 148.04167 | 21.72033 | 2124054 | CHAKRABORTY | 145 | SDSSJ1201+30 | 2 | N | 180.4 | 30.05153 | 2124054 | CHAKRABORTY | 146 | SDSSJ1311 | 2 | N | 197.84167 | -1.39611 | 2124054 | CHAKRABORTY | 147 | SDSSJ1323 | 2 | N | 200.925 | 48.45036 | 2124054 | CHAKRABORTY | 148 | SDSSJ1342 | 2 | N | 205.68333 | 5.51558 | 2124054 | CHAKRABORTY | 149 | SDSSJ1350 | 2 | N | 207.50833 | 29.26936 | 2124054 | CHAKRABORTY | 150 | SN2017BCC | 2 | N | 172.97083 | 29.99578 | 2124054 | CHAKRABORTY | 151 | SWIFT J1112-82 | 2 | N | 167.95 | -82.64583 | 2124054 | CHAKRABORTY | 152 | SWIFT J1644+57 | 2 | N | 251.20417 | 57.58083 | 2124054 | CHAKRABORTY | 153 | SWIFT J2058+05 | 2 | N | 314.58333 | 5.22583 | 2124054 | CHAKRABORTY | 154 | TDE2 | 2 | N | 350.95417 | -1.13611 | 2124054 | CHAKRABORTY | 155 | UGC 01791 | 2 | N | 34.975 | 28.24794 | 2124054 | CHAKRABORTY | 156 | UGC 03317 | 2 | N | 83.40833 | 73.72397 | 2124054 | CHAKRABORTY | 157 | WINGS J134849.88+263 | 2 | N | 207.20833 | 26.59931 | 2124054 | CHAKRABORTY | 158 | XMMSL1 J024916.6-041 | 2 | N | 42.31917 | -4.21222 | 2124054 | CHAKRABORTY | 159 | XMMSL1 J111527.3+180 | 2 | N | 168.86375 | 18.11056 | 2124054 | CHAKRABORTY | 160 | XMMSL1 J132342.3+482 | 2 | N | 200.92625 | 48.45028 | 2124054 | CHAKRABORTY | 161 | XMMSL1 J093922.5+370 | 2 | N | 144.84375 | 37.1625 | 2124054 | CHAKRABORTY | 162 | XMMSL1 J020303.1-074 | 2 | N | 30.76292 | -7.69833 | 2124054 | CHAKRABORTY | 163 | XMMSL1 J061927.1-655 | 2 | N | 94.86292 | -65.88639 | 2124054 | CHAKRABORTY | 164 | XMMSL1 J063045.9-603 | 2 | N | 115.03333 | 85.6575 | 2124054 | CHAKRABORTY | 165 | XMMSL1 J074008.2-853 | 2 | N | 115.03417 | -85.6575 | 2124054 | CHAKRABORTY | 166 | XMMSL1 J131952.3+225 | 2 | N | 97.69167 | -60.51944 | 2124054 | CHAKRABORTY | 167 | XMMSL2 J140446.9-251 | 2 | N | 211.19583 | -25.19306 | 2124054 | CHAKRABORTY | 168 | XMMSL2 J144605.0+685 | 2 | N | 221.52083 | 68.95861 | 2124054 | CHAKRABORTY | 169 | SDSS J143359.16+4006 | 2 | N | 218.4965 | 40.11 | 2124054 | CHAKRABORTY | 170 | ATLAS18MLW | 2 | N | 113.93683 | 66.62147 | 2124054 | CHAKRABORTY | 171 | ERASST J074426.3+291 | 2 | N | 116.10888 | 29.26872 | 2124054 | CHAKRABORTY | 172 | ERASST J0456 | 2 | N | 74.20958 | -20.63056 | 2124054 | CHAKRABORTY | 173 | SDSS J152717.95+1645 | 2 | N | 231.82479 | 16.75081 | 2124054 | CHAKRABORTY | 174 | AT2018CQH | 2 | N | 38.44554 | -1.02456 | 2124054 | CHAKRABORTY | 175 | RX J133157.6-324319. | 2 | N | 202.99058 | -32.72219 | 2124054 | CHAKRABORTY | 176 | SDSS J134244.4+05305 | 2 | N | 205.68508 | 5.51558 | 2124054 | CHAKRABORTY | 177 | T1 (2MASX J00414632-) | 2 | N | 10.443 | -28.46178 | 2124054 | CHAKRABORTY | 178 | T2 (GAMA 91637) | 2 | N | 212.87583 | 0.47211 | 2124054 | CHAKRABORTY | 179 | T3 (XXL-AAOMEGA) J234 | 2 | N | 355.73308 | -54.49961 | 2124054 | CHAKRABORTY | 180 | T4 (SDSS J152717.95+) | 2 | N | 231.82479 | 16.75086 | 2124054 | CHAKRABORTY | 181 | AT2023LLI | 2 | N | 344.41446 | 40.54444 | 2124054 | CHAKRABORTY | 182 | SDSS J143359.16+4006 | 2 | N | 218.4965 | 40.11 | 2124054 | CHAKRABORTY | 183 | ZTF19ACNSKYY | 2 | N | 203.83329 | 7.46819 | 2124058 | WANG | 1 | POX 52 | 40 | N | 180.73721 | -20.93417 | 2124061 | VAN DEN EIJNDEN | 1 | TRANSIENT BEXRB | 20 | Y | 0 | 0 | 2124062 | PENIL | 1 | PG 1553+113 | 12 | N | 238.93171 | 11.18767 | 2124064 | NUNEZ | 1 | URAT1-659242246 | 2 | N | 244.02321 | 41.73656 | 2124064 | NUNEZ | 2 | URAT1-674239311 | 13 | N | 244.46375 | 44.78003 | 2124064 | NUNEZ | 3 | BD+49 2434 | 2 | N | 238.64988 | 49.39544 | 2124064 | NUNEZ | 4 | URAT1-707244162 | 16 | N | 251.45258 | 51.21631 | 2124064 | NUNEZ | 5 | URAT1-715249269 | 12 | N | 253.89125 | 52.87233 | 2124064 | NUNEZ | 6 | URAT1-722250044 | 7 | N | 255.73025 | 54.34072 | 2124064 | NUNEZ | 7 | URAT1-721250635 | 15 | N | 252.48813 | 54.03517 | 2124064 | NUNEZ | 8 | TYC 3040-883-1 | 3 | N | 211.22808 | 42.92378 | 2124064 | NUNEZ | 9 | URAT1-687234652 | 29 | N | 213.12117 | 47.37925 | 2124064 | NUNEZ | 10 | UCAC4 707-051910 | 17 | N | 209.59942 | 51.37844 | 2124064 | NUNEZ | 11 | URAT1-711236225 | 4 | N | 208.65225 | 52.01122 | 2124064 | NUNEZ | 12 | URAT1-713234608 | 7 | N | 201.34025 | 52.42244 | 2124064 | NUNEZ | 13 | URAT1-752231101 | 15 | N | 197.86138 | 60.20553 | 2124064 | NUNEZ | 14 | TYC 3489-1148-1 | 5 | N | 234.46004 | 51.53769 | 2124064 | NUNEZ | 15 | URAT1-739244050 | 9 | N | 234.45646 | 57.68433 | 2124064 | NUNEZ | 16 | UCAC4 714-052491 | 13 | N | 220.73492 | 52.68367 | 2124064 | NUNEZ | 17 | TYC 3861-1374-1 | 3 | N | 222.52367 | 53.63483 | 2124064 | NUNEZ | 18 | HD 238351 | 2 | N | 216.29642 | 57.63322 | 2124064 | NUNEZ | 19 | UCAC4 744-049386 | 7 | N | 222.57475 | 58.68911 | 2124064 | NUNEZ | 20 | HD 238423 | 2 | N | 225.82025 | 59.01153 | 2124064 | NUNEZ | 21 | TYC 3867-1373-1 | 7 | N | 222.87608 | 59.53208 | 2124064 | NUNEZ | 22 | URAT1-751232663 | 6 | N | 217.69417 | 60.19039 | 2124064 | NUNEZ | 23 | TYC 4173-609-1 | 3 | N | 219.82017 | 61.93128 | 2124064 | NUNEZ | 24 | TYC 4183-927-1 | 3 | N | 226.22817 | 63.74164 | 2124064 | NUNEZ | 25 | TIC 198204954 | 10 | N | 246.80504 | 62.96806 | 2124064 | NUNEZ | 26 | TYC 4164-274-1 | 8 | N | 204.86362 | 61.06175 | 2124064 | NUNEZ | 27 | TYC 4174-1117-1 | 9 | N | 209.67142 | 63.68878 | 2124064 | NUNEZ | 28 | HD 234061 | 2 | N | 205.40225 | 53.33753 | 2124064 | NUNEZ | 29 | TYC 3877-725-1 | 3 | N | 240.27854 | 53.41639 | 2124064 | NUNEZ | 30 | TYC 3471-333-1 | 3 | N | 210.58983 | 52.41775 | 2124068 | KENNEA | 1 | GW EM CANDIDATE #1 | 70 | Y | 0 | 0 | 2124068 | KENNEA | 2 | GW EM CANDIDATE #2 | 70 | Y | 0 | 0 | 2124068 | KENNEA | 3 | GW EM CANDIDATE #3 | 70 | Y | 0 | 0 | 2124072 | WOODWARD | 1 | T CRB | 28 | Y | 239.87567 | 25.92017 | 2124072 | WOODWARD | 2 | T CRB | 80 | Y | 239.87567 | 25.92017 | 2124072 | WOODWARD | 3 | T CRB | 12 | Y | 239.87567 | 25.92017 | 2124072 | WOODWARD | 4 | T CRB | 26 | Y | 239.87567 | 25.92017 | 2124077 | EDELSON | 1 | NGC 4151 | 53 | N | 182.63575 | 39.40586 | 2124078 | KENNEA | 1 | ICECUBE TRIGGER #1 | 9.5 | Y | 0 | 0 | 2124078 | KENNEA | 2 | ICECUBE TRIGGER #2 | 9.5 | Y | 0 | 0 | 2124078 | KENNEA | 3 | ICECUBE TRIGGER #3 | 18.5 | Y | 0 | 0 | 2124078 | KENNEA | 4 | KM3NET TRIGGER #1 | 3.5 | Y | 0 | 0 | 2124078 | KENNEA | 5 | KM3NET TRIGGER #2 | 9.5 | Y | 0 | 0 | 2124078 | KENNEA | 6 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2124078 | KENNEA | 7 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2124078 | KENNEA | 8 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2124078 | KENNEA | 9 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2124078 | KENNEA | 10 | NEUTRINO CANDIDATE | 1 | Y | 0 | 0 | 2124087 | DEGENAAR | 1 | VFXT-1 | 25 | Y | 0 | 0 | 2124087 | DEGENAAR | 2 | VFXT-2 | 25 | Y | 0 | 0 | 2124095 | MARGUTTI | 1 | SLSN1 | 110 | Y | 0 | 0 | 2124095 | MARGUTTI | 2 | SLSN2 | 110 | Y | 0 | 0 | 2124097 | MARGUTTI | 1 | FBOT | 90 | Y | 0 | 0 | 2124113 | AUCHETTL | 1 | BH-TDE | 62 | Y | 0 | 0 | 2124115 | BORGHESE | 1 | MAGNETAR OUTBURST | 45 | Y | 0 | 0 | 2124119 | FUERST | 1 | NGC 7793 P13 | 41 | N | 359.46254 | -32.62406 | 2124127 | MASTERSON | 1 | WTP15ABUPKT | 2 | N | 242.77379 | 2.56675 | 2124127 | MASTERSON | 2 | WTP16AAVEGO | 2 | N | 161.50658 | -36.30236 | 2124127 | MASTERSON | 3 | WTP15ABZOOA | 2 | N | 254.36171 | 23.75783 | 2124127 | MASTERSON | 4 | WTP17AANKKJ | 2 | N | 178.52088 | -5.83333 | 2124127 | MASTERSON | 5 | WTP16AASRAL | 2 | N | 10.93592 | -33.944 | 2124127 | MASTERSON | 6 | WTP10ACPIKA | 2 | N | 80.44062 | -30.29619 | 2124127 | MASTERSON | 7 | WTP17AAKTGS | 2 | N | 13.94962 | -61.60772 | 2124127 | MASTERSON | 8 | WTP11AADIVN | 2 | N | 55.43542 | -53.70597 | 2124127 | MASTERSON | 9 | WTP10ACPIKA | 2 | N | 80.44062 | -30.29619 | 2124127 | MASTERSON | 10 | WTP17AALMPS | 2 | N | 15.835 | 14.03125 | 2124127 | MASTERSON | 11 | WTP17AAHYUS | 2 | N | 96.44021 | -4.36783 | 2124127 | MASTERSON | 12 | WTP14ADCCAD | 2 | N | 203.14129 | 44.39344 | 2124127 | MASTERSON | 13 | WTP17AAMOXE | 2 | N | 317.24237 | -56.47533 | 2124127 | MASTERSON | 14 | WTP14ADCADY | 2 | N | 9.78654 | -23.98792 | 2124127 | MASTERSON | 15 | WTP10ADERAJ | 2 | N | 310.32421 | -45.15436 | 2124127 | MASTERSON | 16 | WTP11AADGEF | 2 | N | 234.29712 | 58.23894 | 2124127 | MASTERSON | 17 | WTP17AANASC | 2 | N | 147.84437 | 22.12125 | 2124127 | MASTERSON | 18 | WTP17AAEAKZ | 2 | N | 157.58004 | -47.31086 | 2124127 | MASTERSON | 19 | WTP16AAPEIB | 2 | N | 210.58858 | 39.36969 | 2124127 | MASTERSON | 20 | WTP17AALMRA | 2 | N | 197.31808 | -44.77981 | 2124127 | MASTERSON | 21 | WTP14ADALRP | 2 | N | 125.126 | -5.08014 | 2124127 | MASTERSON | 22 | WTP17AALTJC | 2 | N | 219.26796 | -40.08967 | 2124127 | MASTERSON | 23 | WTP15ABYRAK | 2 | N | 215.7255 | 6.16489 | 2124127 | MASTERSON | 24 | WTP17AAJCJL | 2 | N | 36.72146 | 41.69031 | 2124127 | MASTERSON | 25 | WTP15ABXFYC | 2 | N | 314.33442 | 12.21256 | 2124127 | MASTERSON | 26 | WTP15ABXQUS | 2 | N | 168.90238 | 5.74717 | 2124127 | MASTERSON | 27 | WTP15ABWFGK | 2 | N | 136.91133 | 56.73281 | 2124127 | MASTERSON | 28 | WTP16AARLOY | 2 | N | 323.19696 | -60.29908 | 2124127 | MASTERSON | 29 | WTP18AAKFQB | 2 | N | 252.15825 | 1.47078 | 2124127 | MASTERSON | 30 | WTP15ACCELY | 2 | N | 174.13721 | -29.09067 | 2124127 | MASTERSON | 31 | WTP15ABVDFA | 2 | N | 89.79704 | -31.4425 | 2124127 | MASTERSON | 32 | WTP15ACBUUV | 2 | N | 154.67258 | -13.00189 | 2124127 | MASTERSON | 33 | WTP16AASVGC | 2 | N | 174.40692 | -43.32983 | 2124127 | MASTERSON | 34 | WTP14ADEQKA | 2 | N | 297.3535 | 63.50919 | 2124127 | MASTERSON | 35 | WTP16AAPTDI | 2 | N | 229.68646 | -21.94622 | 2124127 | MASTERSON | 36 | WTP10AATEAL | 2 | N | 115.64196 | 8.85739 | 2124127 | MASTERSON | 37 | WTP16AARCXP | 2 | N | 138.87933 | 48.23547 | 2124127 | MASTERSON | 38 | WTP15ABYGFC | 2 | N | 200.01633 | 7.71642 | 2124127 | MASTERSON | 39 | WTP16AAPBLL | 2 | N | 331.87413 | 49.516 | 2124127 | MASTERSON | 40 | WTP14ACZRAI | 2 | N | 328.64329 | -70.02436 | 2124127 | MASTERSON | 41 | WTP18AAMPWJ | 2 | N | 26.67683 | 32.50814 | 2124127 | MASTERSON | 42 | WTP15ABUQNJ | 2 | N | 68.732 | -0.69592 | 2124127 | MASTERSON | 43 | WTP14ACKXCR | 2 | N | 48.82067 | -16.43378 | 2124127 | MASTERSON | 44 | WTP19AALJMZ | 2 | N | 359.79663 | 1.16856 | 2124127 | MASTERSON | 45 | WTP18AANJWC | 2 | N | 99.39171 | 69.15233 | 2124127 | MASTERSON | 46 | WTP16AAPTJA | 2 | N | 237.91892 | 8.87392 | 2124127 | MASTERSON | 47 | WTP15AAEPOL | 2 | N | 63.76779 | 36.72397 | 2124127 | MASTERSON | 48 | WTP17AALWZI | 2 | N | 251.97658 | 38.72833 | 2124127 | MASTERSON | 49 | WTP14ADAOYA | 2 | N | 6.97225 | -69.02739 | 2124127 | MASTERSON | 50 | WTP18AADMEZ | 2 | N | 132.54142 | -31.63397 | 2124127 | MASTERSON | 51 | WTP14ACZNJM | 2 | N | 209.62788 | 81.07633 | 2124127 | MASTERSON | 52 | WTP17AAKTRS | 2 | N | 171.19271 | 4.92383 | 2124127 | MASTERSON | 53 | WTP15ACALBW | 2 | N | 99.23825 | 47.03547 | 2124127 | MASTERSON | 54 | WTP16AASFKY | 2 | N | 343.6745 | -27.89692 | 2124127 | MASTERSON | 55 | WTP15ABUYJP | 2 | N | 17.04904 | 85.69742 | 2124127 | MASTERSON | 56 | WTP18AAOMJE | 2 | N | 267.83425 | 52.54569 | 2124127 | MASTERSON | 57 | WTP17AALMRA | 2 | N | 197.31808 | -44.77981 | 2124127 | MASTERSON | 58 | WTP19AANQHX | 2 | N | 336.99354 | 18.32181 | 2124127 | MASTERSON | 59 | WTP15ACBGPN | 2 | N | 166.25825 | 59.68436 | 2124127 | MASTERSON | 60 | WTP19AAKRAI | 2 | N | 314.26237 | 14.20453 | 2124127 | MASTERSON | 61 | WTP15ABYYCQ | 2 | N | 237.48 | 33.46444 | 2124127 | MASTERSON | 62 | WTP17AALBEK | 2 | N | 202.25858 | 23.68569 | 2124127 | MASTERSON | 63 | WTP16AASYCR | 2 | N | 201.93421 | -5.48014 | 2124127 | MASTERSON | 64 | WTP18AAJWVZ | 2 | N | 220.94767 | -39.41497 | 2124127 | MASTERSON | 65 | WTP18AACYGY | 2 | N | 285.23854 | -24.4 | 2124127 | MASTERSON | 66 | WTP14ACTLWY | 2 | N | 6.62358 | 37.64733 | 2124127 | MASTERSON | 67 | WTP15ABYMDQ | 2 | N | 57.21987 | -55.42639 | 2124127 | MASTERSON | 68 | WTP16AAVEUO | 2 | N | 184.78287 | 5.27933 | 2124127 | MASTERSON | 69 | WTP19AAJIKW | 2 | N | 234.22121 | 31.85436 | 2124127 | MASTERSON | 70 | WTP15AASXBN | 2 | N | 115.96896 | -24.84942 | 2124127 | MASTERSON | 71 | WTP15ACCARC | 2 | N | 347.06937 | 37.70294 | 2124127 | MASTERSON | 72 | WTP15ABVPLV | 2 | N | 111.04467 | 27.89961 | 2124127 | MASTERSON | 73 | WTP18AAJKMK | 2 | N | 40.099 | -2.72825 | 2124127 | MASTERSON | 74 | WTP17AALMSG | 2 | N | 222.12063 | 11.62558 | 2124127 | MASTERSON | 75 | WTP17AALZPX | 2 | N | 50.85696 | -2.04678 | 2124127 | MASTERSON | 76 | WTP17AALMSG | 2 | N | 222.12063 | 11.62558 | 2124127 | MASTERSON | 77 | WTP17AANAWB | 2 | N | 137.76208 | -9.62042 | 2124127 | MASTERSON | 78 | WTP17AALQGV | 2 | N | 31.71413 | -11.22822 | 2124127 | MASTERSON | 79 | WTP14ABNPGK | 2 | N | 251.47767 | -23.45175 | 2124127 | MASTERSON | 80 | WTP16AATSNW | 2 | N | 254.84442 | 20.82983 | 2124127 | MASTERSON | 81 | WTP10ACJNVQ | 2 | N | 131.61433 | -59.16278 | 2124127 | MASTERSON | 82 | WTP14ACKODC | 2 | N | 207.02492 | 7.38753 | 2124127 | MASTERSON | 83 | WTP16AAPICT | 2 | N | 26.24958 | 28.09192 | 2124127 | MASTERSON | 84 | WTP14ACZAKM | 2 | N | 96.8225 | -35.21411 | 2124127 | MASTERSON | 85 | WTP16AAUBRH | 2 | N | 274.01183 | 36.614 | 2124127 | MASTERSON | 86 | WTP15ABZMAS | 2 | N | 70.47338 | -39.77547 | 2124127 | MASTERSON | 87 | WTP15ABTXZI | 2 | N | 223.43029 | 27.31717 | 2124127 | MASTERSON | 88 | WTP14ACSTBQ | 2 | N | 351.22067 | 37.21539 | 2124127 | MASTERSON | 89 | WTP15ABXJTH | 2 | N | 10.37329 | -63.15933 | 2124127 | MASTERSON | 90 | WTP17AAKWRK | 2 | N | 190.73071 | 25.62442 | 2124127 | MASTERSON | 91 | WTP17AAMGRX | 2 | N | 269.74142 | 39.86817 | 2124127 | MASTERSON | 92 | WTP14ACHYBJ | 2 | N | 133.39546 | -28.16803 | 2124127 | MASTERSON | 93 | WTP15ABVFJG | 2 | N | 97.325 | 66.79094 | 2124127 | MASTERSON | 94 | WTP14ACYEWQ | 2 | N | 269.97642 | 24.29225 | 2124127 | MASTERSON | 95 | WTP17AAIMNJ | 2 | N | 124.33075 | -24.23733 | 2124127 | MASTERSON | 96 | WTP14ACKVUX | 2 | N | 244.58513 | 52.51406 | 2124127 | MASTERSON | 97 | WTP17AAMZEW | 2 | N | 146.23583 | 31.09794 | 2124127 | MASTERSON | 98 | WTP14ACZAJV | 2 | N | 105.36433 | 59.27106 | 2124127 | MASTERSON | 99 | WTP15ABYIWQ | 2 | N | 19.58429 | -15.26375 | 2124127 | MASTERSON | 100 | WTP17AAMSXP | 2 | N | 126.49067 | 45.2525 | 2124127 | MASTERSON | 101 | WTP16AAQRCR | 2 | N | 280.83067 | -62.11225 | 2124127 | MASTERSON | 102 | WTP14AAMFEK | 2 | N | 85.92067 | 31.70522 | 2124127 | MASTERSON | 103 | WTP14ADAXZI | 2 | N | 156.57913 | 45.578 | 2124127 | MASTERSON | 104 | WTP17AAHSZT | 2 | N | 90.64404 | 49.60322 | 2124127 | MASTERSON | 105 | WTP14ADAQLC | 2 | N | 135.73067 | 19.58358 | 2124127 | MASTERSON | 106 | WTP15ACDELM | 2 | N | 236.40329 | 70.72547 | 2124127 | MASTERSON | 107 | WTP16AATVBU | 2 | N | 260.58358 | 31.74353 | 2124127 | MASTERSON | 108 | WTP16AAVCPT | 2 | N | 11.25213 | -0.78978 | 2124127 | MASTERSON | 109 | WTP17AANBSO | 2 | N | 180.90971 | 58.98656 | 2124127 | MASTERSON | 110 | WTP15ABZDPE | 2 | N | 47.13192 | -0.83603 | 2124127 | MASTERSON | 111 | WTP18AAJQQD | 2 | N | 232.9645 | 37.41275 | 2124127 | MASTERSON | 112 | WTP14ADBJSH | 2 | N | 342.95317 | -20.60803 | 2124127 | MASTERSON | 113 | WTP15ABTYCD | 2 | N | 188.92863 | -47.22739 | 2124127 | MASTERSON | 114 | WTP17AAIOSN | 2 | N | 304.29663 | 58.20253 | 2124127 | MASTERSON | 115 | WTP15AAXNAV | 2 | N | 150.87908 | -44.39189 | 2124127 | MASTERSON | 116 | WTP14ADBQMD | 2 | N | 169.46942 | 29.30453 | 2124135 | SIEGEL | 1 | NGC 4147 | 6 | N | 182.52562 | 18.54217 | 2124135 | SIEGEL | 2 | NGC4372 | 4 | N | 186.43929 | -72.65908 | 2124135 | SIEGEL | 3 | NGC 5466 | 6 | N | 211.36371 | 28.53444 | 2124135 | SIEGEL | 4 | NGC 5824 | 6 | N | 225.99421 | -33.06853 | 2124135 | SIEGEL | 5 | PALOMAR 5 | 6 | N | 229.02208 | -0.11139 | 2124135 | SIEGEL | 6 | M5 | 4 | N | 229.63842 | 2.08103 | 2124135 | SIEGEL | 7 | NGC 6139 | 6 | N | 246.91662 | -38.84917 | 2124135 | SIEGEL | 8 | NGC 6284 | 6 | N | 256.11979 | -24.76422 | 2124135 | SIEGEL | 9 | NGC 6304 | 2 | N | 258.63437 | -29.46203 | 2124135 | SIEGEL | 10 | NGC 6325 | 6 | N | 259.49696 | -23.76603 | 2124135 | SIEGEL | 11 | NGC 6355 | 6 | N | 260.99437 | -26.35342 | 2124135 | SIEGEL | 12 | NGC 6401 | 6 | N | 264.65387 | -23.90875 | 2124135 | SIEGEL | 13 | NGC 6426 | 6 | N | 266.22796 | 3.17014 | 2124135 | SIEGEL | 14 | NGC 6453 | 2 | N | 267.71571 | -34.59864 | 2124135 | SIEGEL | 15 | NGC 6522 | 2 | N | 270.892 | -30.03397 | 2124135 | SIEGEL | 16 | NGC 6528 | 2 | N | 271.20671 | -30.05578 | 2124135 | SIEGEL | 17 | NGC 6558 | 4 | N | 272.57079 | -31.76389 | 2124135 | SIEGEL | 18 | NGC 6569 | 2 | N | 273.412 | -31.82644 | 2124135 | SIEGEL | 19 | NGC 6638 | 2 | N | 277.73438 | -25.49642 | 2124135 | SIEGEL | 20 | PALOMAR 8 | 4 | N | 280.37458 | -19.82583 | 2124137 | GAUDIN | 1 | BE/X-RAY BINARIES | 170 | Y | 0 | 0 | 2124146 | SOKOLOSKI | 1 | T CRB | 88 | N | 239.87567 | 25.92017 | 2124152 | RAJGURU | 1 | 5BZQ J1242+3751 | 8 | N | 190.714 | 37.85 | 2124152 | RAJGURU | 2 | 5BZQ J0728-4745 | 50 | N | 112.09796 | -47.75472 | 2124152 | RAJGURU | 3 | 5BZQ J1509-4340 | 8 | N | 227.39871 | -43.67558 | 2124152 | RAJGURU | 4 | 5BZQ J0721+0406 | 5 | N | 110.34958 | 4.11228 | 2124152 | RAJGURU | 5 | 5BZQ J0239+0416 | 4 | N | 39.96354 | 4.27261 | 2124152 | RAJGURU | 6 | 5BZQ J0029+0509 | 26 | N | 7.26492 | 5.15967 | 2124156 | BODEWITS | 1 | C2023A3 | 36 | N | 0 | 0 | 2124156 | BODEWITS | 2 | C2024E1 | 73.8 | N | 0 | 0 | 2124165 | MARCULEWICZ | 1 | J083650.86+142539.0 | 10 | N | 129.21196 | 14.4275 | 2124165 | MARCULEWICZ | 2 | J094533.98+100950.1 | 4 | N | 146.39163 | 10.16392 | 2124165 | MARCULEWICZ | 3 | J114153.34+021924.3 | 10 | N | 175.47225 | 2.32342 | 2124165 | MARCULEWICZ | 4 | J123743.08+630144.9 | 10 | N | 189.4295 | 63.02914 | 2124165 | MARCULEWICZ | 5 | J141141.96+140233.9 | 10 | N | 212.92483 | 14.04278 | 2124165 | MARCULEWICZ | 6 | J141730.92+073320.7 | 10 | N | 214.37887 | 7.55575 | 2124165 | MARCULEWICZ | 7 | J144741.76-020339.1 | 10 | N | 221.92404 | -2.06089 | 2124165 | MARCULEWICZ | 8 | J152156.48+520238.5 | 1 | N | 230.48533 | 52.04406 | 2124165 | MARCULEWICZ | 9 | PG1407+265 | 1 | N | 212.34963 | 26.30586 | 2124177 | VIELIUTE | 1 | I ZW 1 | 5 | N | 13.39554 | 12.69331 | 2124177 | VIELIUTE | 2 | NGC 3783 | 5 | N | 174.75713 | -37.73861 | 2124177 | VIELIUTE | 3 | NGC 4051 | 5 | N | 180.79004 | 44.53131 | 2124177 | VIELIUTE | 4 | PG 0804+761 | 5 | N | 122.74442 | 76.04514 | 2124177 | VIELIUTE | 5 | MRK 493 | 5 | N | 239.79008 | 35.02989 | 2124177 | VIELIUTE | 6 | MRK 766 | 5 | N | 184.6105 | 29.81292 | 2124177 | VIELIUTE | 7 | MCG-6-30-15 | 5 | N | 203.97404 | -34.29561 | 2124177 | VIELIUTE | 8 | PDS 456 | 5 | N | 262.08246 | -14.26553 | 2124177 | VIELIUTE | 9 | ARK 564 | 5 | N | 340.66392 | 29.72536 | 2124184 | KAPLAN | 1 | VAST 1 | 5 | Y | 0 | 0 | 2124184 | KAPLAN | 2 | VAST 1 | 5 | Y | 0 | 0 | 2124184 | KAPLAN | 3 | VAST 1 | 5 | Y | 0 | 0 | 2124184 | KAPLAN | 4 | VAST 1 | 5 | Y | 0 | 0 | 2124185 | MOONEY | 1 | VER J0521+211 | 60 | N | 80.44154 | 21.21431 | 2124187 | SAND | 1 | SMDG1309458 | 3 | N | 197.44071 | -23.54261 | 2124187 | SAND | 2 | SMDG0040146 | 3.3 | N | 10.06092 | -17.82592 | 2124187 | SAND | 3 | SMDG0427280 | 3.3 | N | 66.86654 | -54.97056 | 2124187 | SAND | 4 | SMDG0403293 | 2.5 | N | 67.62225 | -54.65575 | 2124187 | SAND | 5 | SMDG0510457 | 2.8 | N | 77.69025 | -2.76042 | 2124187 | SAND | 6 | SMDG0548400 | 3 | N | 87.16654 | -30.71253 | 2124187 | SAND | 7 | SMDG0609099 | 3.2 | N | 92.29129 | -32.42286 | 2124187 | SAND | 8 | SMDG0614014 | 2.5 | N | 93.50588 | -51.54497 | 2124187 | SAND | 9 | SMDG0624366 | 3.1 | N | 96.15254 | -40.57933 | 2124187 | SAND | 10 | SMDG0705198 | 2.5 | N | 106.33246 | -58.53442 | 2124187 | SAND | 11 | SMDG07210216 | 3.2 | N | 107.59017 | -63.56803 | 2124187 | SAND | 12 | SMDG1043183 | 3.4 | N | 160.82625 | -33.63464 | 2124187 | SAND | 13 | SMDG1123135 | 3.2 | N | 170.80612 | 13.71478 | 2124187 | SAND | 14 | SMDG1143104 | 2.7 | N | 175.79342 | 14.2235 | 2124187 | SAND | 15 | SMDG1302221 | 3.5 | N | 195.59196 | -4.50128 | 2124187 | SAND | 16 | SMDG2232419 | 2.5 | N | 338.17446 | 31.22022 | 2124187 | SAND | 17 | SMDG1309458 | 3.5 | N | 178.02346 | 54.79247 | 2124187 | SAND | 18 | SMDG1235016 | 2.9 | N | 188.75679 | 58.38642 | 2124187 | SAND | 19 | SMDG0427313 | 3.4 | N | 66.88058 | -54.93181 | 2124187 | SAND | 20 | SMDG1309458 | 3.2 | N | 67.58713 | -13.483 | 2124187 | SAND | 21 | SMDG1851103 | 2.9 | N | 282.79292 | -64.008 | 2124187 | SAND | 22 | SMDG0320181 | 2.7 | N | 50.07521 | -25.69731 | 2124192 | LINCETTO | 1 | KM3NET TOO 1 | 14 | Y | 0 | 0 | 2124192 | LINCETTO | 2 | KM3NET TOO 2 | 14 | Y | 0 | 0 | 2124198 | MCBRIDE | 1 | NEUTRINO ALERT 1 | 4.5 | Y | 0 | 0 | 2124198 | MCBRIDE | 2 | NEUTRINO ALERT 2 | 4.5 | Y | 0 | 0 | 2124198 | MCBRIDE | 3 | NEUTRINO ALERT 3 | 4.5 | Y | 0 | 0 | 2124198 | MCBRIDE | 4 | NEUTRINO ALERT 4 | 4.5 | Y | 0 | 0 | 2124203 | CLARK | 1 | HGGK681 | 37.9 | N | 210.8025 | 54.59494 | 2124203 | CLARK | 2 | NGC5471 | 6 | N | 211.11929 | 54.398 | 2124205 | HOSSEINZADEH | 1 | SN1 | 36 | Y | 0 | 0 | 2124205 | HOSSEINZADEH | 2 | SN2 | 36 | Y | 0 | 0 | 2124205 | HOSSEINZADEH | 3 | SN3 | 36 | Y | 0 | 0 | 2124205 | HOSSEINZADEH | 4 | SN4 | 36 | Y | 0 | 0 | 2124205 | HOSSEINZADEH | 5 | SN5 | 36 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 1 | INFANT TDE TOO | 62 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 2 | INFANT TDE TOO | 2 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 3 | INFANT TDE TOO | 2 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 4 | INFANT TDE TOO | 2 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 5 | INFANT TDE TOO | 2 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 6 | INFANT TDE TOO | 2 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 7 | INFANT TDE TOO | 2 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 8 | INFANT TDE TOO | 2 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 9 | INFANT TDE TOO | 2 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 10 | INFANT TDE TOO | 2 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 11 | INFANT TDE TOO | 62 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 12 | INFANT TDE TOO | 22 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 13 | INFANT TDE TOO | 22 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 14 | INFANT TDE TOO | 22 | Y | 0 | 0 | 2124207 | HAMMERSTEIN | 15 | INFANT TDE TOO | 22 | Y | 0 | 0 | 2124211 | LIN | 1 | HLX-1_2MASXJ0111-45 | 36 | N | 17.69583 | -46.02556 | 2124212 | LAWTHER | 1 | MRK 590 | 99 | N | 33.63983 | -0.76672 | 2124218 | WALSH | 1 | MRK 590 | 54 | N | 33.63983 | -0.76672 | 2124237 | SANTANDER | 1 | FERMI_HEP_1 | 4 | Y | 0 | 0 | 2124237 | SANTANDER | 2 | FERMI_HEP_2 | 4 | Y | 0 | 0 | 2124237 | SANTANDER | 3 | FERMI_HEP_3 | 4 | Y | 0 | 0 | 2124237 | SANTANDER | 4 | FERMI_HEP_4 | 4 | Y | 0 | 0 | 2124237 | SANTANDER | 5 | FERMI_HEP_5 | 4 | Y | 0 | 0 | 2124237 | SANTANDER | 6 | FERMI_HEP_6 | 4 | Y | 0 | 0 | 2124237 | SANTANDER | 7 | FERMI_HEP_7 | 4 | Y | 0 | 0 | 2124237 | SANTANDER | 8 | FERMI_HEP_8 | 4 | Y | 0 | 0 | 2124237 | SANTANDER | 9 | FERMI_HEP_9 | 4 | Y | 0 | 0 | 2124237 | SANTANDER | 10 | FERMI_HEP_10 | 4 | Y | 0 | 0 | 2124240 | WARD | 1 | J031224-4353.9 | 40 | N | 48.10129 | -43.89836 | 2124240 | WARD | 2 | J212159-4530.5 | 170 | N | 320.49821 | -45.51 |
Proposal Abstracts
2124005 / LAHA / UNIVERSITY OF MARYLAND (BALTIMORE COUNTY)
"CAUGHT IN THE ACT: A SWIFT TOO CAMPAIGN ON CHANGING-LOOK AGN"
Changing look active galactic nuclei (CL-AGNs) show extreme variations in the optical, UV, and X-ray luminosity in timescales spanning months to years. It seems likely that CL-AGN events are driven by rapid and extreme changes in the accretion disk around the super-massive black hole (SMBH), which also affects the coronal emission causing large unexplained variations in 0.3-2 and 2-10 keV flux and spectral states. The CL-AGN are therefore ideal test beds to understand the properties of coronal X-ray emission, and its relation with the accretion disk (UV). To achieve this, the proposal aims to densely monitor the X-ray+UV emission from a CL-AGN in its initial phase of outburst. Swift with its simultaneous X-ray+UV observational capability is uniquely suited for this experiment
2124009 / 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.
2124011 / PERNA / STATE UNIVERSITY OF NEW YORK AT STONY BROOK
"CALIBRATING THE STELLAR POPULATION IN THE DISKS OF ACTIVE GALACTIC NUCLEI VIA GRB OBSERVATIONS"
With the discovery of gravitational waves, AGN disks have emerged as a potentially interesting environment for hosting some of these sources. AGN disks are conducive to forming both long and short GRBs. However, theoretical predictions for the expected cosmological population of GRBs exploding in the very high ambient density environments specific to AGN disks are missing, effectively preventing the use of this data to constrain the underlying stellar and compact object population, and its contribution to the detected gravitational wave events. Here, by means of Monte Carlo methods coupled with models for GRB light curves in very dense media, we aim at simulating this population, with the goal of creating a link which will allow Swift observations to uncover its intrinsic properties
2124014 / PASHAM / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"SWIFT+NICER OBSERVATIONS TO IDENTIFY AND STUDY COSMOLOGICAL BLACK HOLES TURNING ON RELATIVISTIC JETS"
Following Swift (XRT+UVOT) and NICER's recent success in capturing the spectro-timing variability of the farthest stellar tidal disruption event (TDE) to-date we propose ToO monitoring observations of a future relativistic TDE, i.e., a system with a newborn relativistic jet pointed directly along our line of sight. Our main goals are 1) to establish the relativistic nature of the future transient by measuring its luminosity and variability, and 2) combine NICER and Swift/UVOT data with our approved multi-frequency radio data to perform multi-epoch spectral energy distribution modelings to shed light on the underlying jet physics. Our scientific goals require high-cadence monitoring and optical/UV coverage for months making NICER+Swift ideal for the proposed study.
2124018 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
"SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS IN CYCLE 21"
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.
2124035 / TOIVONEN / UNIVERSITY OF MINNESOTA
"THE LOW-LATENCY GRAVITATIONAL-WAVE ALERT SYSTEM ENABLING SWIFT FOLLOW-UP"
Multi-messenger sources of astrophysical transients are changing the face of time-domain astronomy. Searches for counterparts in other wavelengths and messengers to gamma ray bursts (GRBs) have been relevant to understand their formation processes, including compact binary mergers and collapsars; these include both short and long classes, although this classification is subject to debate. These sources have been identified by GRB survey instruments such as the Neil Gehrels Swift Observatory mission and the Gamma ray Burst Monitor (GBM)) onboard the Fermi satellite.
2124040 / WALTON / UNIVERSITY OF HERTFORDSHIRE
"TESTING THE LENSE-THIRRING MODEL FOR ULX VARIABILITY WITH NGC5907 ULX1"
Following a series of remarkable recent discoveries, it is now clear that some of the ultraluminous X-ray source (ULX) population are actually powered by highly super-Eddington neutron stars. NGC5907 ULX1 is the most extreme of these, exhibiting a remarkable peak luminosity of ~1e41 erg/s, as well as X-ray off-states (where the flux drops by a factor of ~100 or more) and a clear ~78d super-orbital X-ray period when active. Although the source has spent the last ~year in an off-state, it has now returned to its ULX state. This presents a unique opportunity to test the Lense-Thirring interpretation for the super-orbital periods seen in ULX pulsars with continued Swift monitoring.
2124048 / AJELLO / CLEMSON UNIVERSITY
"SWIFT TOOS FOR FERMI GALACTIC PLANE TRANSIENTS"
Fermi has detected hundreds of transients with short (sec to hr) and long (months) variability timescales. However, weekly timescale transients remain mostly unexplored. The Fermi All-sky Variability Analysis (FAVA) allows to systematically search the whole sky for weekly transients. The novelty of FAVA resides in using the mission-long data to provide an estimate of the average sky intensity against which weekly data are compared. This makes FAVA an unbiased and fast tool to find transients in the Galactic plane where the diffuse emission is the brightest. FAVA detects about 7 new galactic transients per year. We propose to use Swift to follow up on the most promising 2. The population of Galactic transients is under-sampled and detecting even 1 new source will have a major impact.
2124051 / HOMAN / EUREKA SCIENTIFIC INC.
"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.
2124054 / CHAKRABORTY / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"UNDERSTANDING THE DIVERSITY OF UNEXPECTED LATE-TIME BEHAVIOR IN TIDAL DISRUPTION EVENTS"
The canonical picture of Tidal Disruption Events (TDEs) suggests the soft X-ray emission should rise on timescales of ∼1 month then decline as t^{-5/3}, but in recent years, X-ray monitoring has revealed they frequently 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). Discovering these is difficult because of the frequent lack of 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 behaviors.
2124058 / WANG / SEOUL NATIONAL UNIVERSITY
"PROBING THE X-RAY REPROCESSING LAG OF A PROTOTYPE INTERMEDIATE-MASS BLACK HOLE IN POX 52"
We request a Swift monitoring of POX 52 using XRT and UVOT. This Dwarf Seyfert 1 galaxy, harboring an intermediate mass black hole (IMBH), exhibits X-ray/UV/optical variabilities. Using the unique capability of Swift for simultaneous and multi-wavelength monitoring, the proposal aims to investigate the correlated variability of X-ray and UV/optical and to detect the lag between these bands. This will provide a unique possibility to test the X-ray reprocessing model in the low-mass regime. Currently, NGC 4395 is the only robust IMBH confirmed through optical reverberation mapping (RM), while POX 52 will be the first IMBH with robust lags from X-ray to UV/optical. Combining with the coordinated continuum and broad-line RM with GTC/Gemini, we will have a comprehensive view of this IMBH.
2124061 / VAN DEN EIJNDEN / UNIVERSITY OF WARWICK
"SWIFT/VLA MONITORING OF THE DECAY OF A GIANT BE/X-RAY BINARY OUTBURST"
The recent discoveries of radio jets produced by highly magnetized neutron stars in Be/X-ray binaries (BeXRBs) is important for several areas of research. Firstly, it has opened up an unexplored parameter regime to study the launching conditions of jets. Secondly, it provides a novel avenue to complement existing X-ray studies to better understand the accretion flow in BeXRBs. We propose 20 ks of Swift monitoring and 6 hr of VLA time to study the decay of a BeXRB giant outburst. The main aims are to i) determine if a sharp transition in the X-ray flux and spectral evolution is common for this class of objects, ii) gain insight into the debated origin of the X-ray emission after this transition, iii) map out the behaviour of the jet in this regime, and its connection to the accretion flow.
2124062 / PENIL / CLEMSON UNIVERSITY
"SWIFT MONITORING OF PG 1553+113, A PERIODICALLY EMITTING BLAZAR"
Blazars show varying emissions across different wavelengths, from minutes to years. We propose using the Swift telescope to observe PG 1553+113, a blazar previously detected in γ-rays with significant periodicity in its lightcurve. These observations will help us understand how the γ-ray, X-ray, and ultraviolet fluxes are related in this periodic blazar. By studying its multiwavelength properties, we aim to uncover the mechanisms driving this phenomenon.
2124064 / NUNEZ / COLUMBIA UNIVERSITY
"COMPLETING 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 complete the observations of 30 low-mass members of Group-X (~100 pc away and ~300 Myr old), which were partly observed as part of the Fill-in Program in Cycle 20. 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.
2124068 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
"KEY PROJECT: THE DETECTION AND MONITORING OF ELECTROMAGNETIC COUNTERPARTS OF GRAVITATIONAL WAVE SOURCES WITH SWIFT IN O4"
We seek to identify and observe EM counterparts to GW events during the final part of the fourth LIGO/Virgo/KAGRA observing run ( O4 ). We request deep follow-up observations at high priority in order to monitor and characterize EM candidates detected by Swift or other observatories. Based on lessons learned during O4, we also propose to greatly enhance the Swift GW follow-up program in preparation of the O5 LVK observing run. These include optimizing the follow-up strategy and trigger criteria, enhancing transient detection abilities by utilizing pre-imaging surveys, searching for prompt emission in BAT data, and adjusting the Swift observing plans according to the the rates and localizations observed during O4.
2124072 / WOODWARD / UNIVERSITY OF MINNESOTA
"THE BRIGHTEST NOVA IN THE LAST 80 YEARS: T CORONAE BOREALIS"
The goal of this proposal is to obtain high S/N, high cadence and multi-wavelength Swift observations during, and after the next eruption of the symbiotic recurrent nova T CrB. Swift's unique x-ray and UV capabilities makes it an ideal instrument to follow what is expected to be the brightest x-ray emitting nova since 1946. T CrB may experience its next nova eruption during Swift AO21. Swift 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. These observations may also explain the unique secondary maximum that occurred ~100 days after the first maximum in 1866 and 1946.
2124077 / EDELSON / EUREKA SCIENTIFIC INC
"INTENSIVE BROADBAND REVERBERATION MAPPING OF NGC 4151"
Intensive Broadband Reverberation Mapping uses interband lags to infer AGN accretion disk properties. NGC 4151, the brightest AGN in the sky, will be monitored with Swift, NICER, and from the ground during 28 Oct 2024-15 Jul 2025. Swift was only approved through Cycle 20, so here we propose to continue daily monitoring until the campaign ends. This will clarify the nature of an earlier anomalous lag spectrum in NGC 4151 based on a 2.3 month campaign in 2016. The addition of NICER allows correlation of UV fluxes with X-ray spectral parameters. The results will provide one of the strongest tests to date of the propagation of fluctuations in the disk, the location of the X/UV reprocessor, and role of BLR emission. Only Swift can provide the UV data necessary to accomplish these goals
2124078 / 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.
2124087 / 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.
2124095 / MARGUTTI / UNIVERSITY OF CALIFORNIA (BERKELEY)
"A PANCHROMATIC INVESTIGATION OF SUPER-LUMINOUS SUPERNOVAE"
Super-luminous Supernovae (SLSNe) can reach peak luminosities that are up to 100 times those of ordinary stellar explosions. After two decades of studies, the nature of the explosion mechanisms and the source of energy powering the exceptional displays of SLSNe are still debated. Progress requires observational guidance. We propose rapid Swift follow up of 2 newly-discovered SLSNe to map the UV and soft X-ray emission during the early evolutionary stages as part of a multi-wavelength effort through programs on the VLA, XMM, Chandra, NuSTAR and optical/NIR facilities. Our goals are to: (i) constrain the energy source and explosion mechanism (e.g., presence of jets); (ii) constrain the diversity of the pre-explosion evolution of their stellar progenitors.
2124097 / MARGUTTI / UNIVERSITY OF CALIFORNIA (BERKELEY)
"CONSTRAINING THE NATURE OF THE MOST EXTREME EXPLOSIVE TRANSIENTS"
Fast and Blue Optical Transients (FBOTs) are a new class of phenomena. With peak luminosities rivaling even those of super-luminous SNe coupled with extremely short rise times of a few days, and evidence for relativistic outflows, FBOTs probe the extremes of the explosion parameters and/or stellar progenitor properties, and are hard to reconcile within standard models. Alternative scenarios include strong shock interaction with a dense medium, or the presence of a central engine. Here we propose a focused Swift investigation of the closest FBOTs (d<300 Mpc) as part of an extensive multi-wavelength monitoring program (radio to X-rays). By densely sampling the UV and X-ray properties of FBOTs with Swift, our overarching goal is to advance our understanding of their intrinsic nature.
2124101 / STRADER / MICHIGAN STATE UNIVERSITY
"HUNTING NEW MILLISECOND PULSAR BINARIES"
JAY STRADER Support is requested for a program to perform follow-up optical spectroscopy of Swift/XRT X-ray sources that are candidate millisecond pulsar binaries. This program presents a unique opportunity to add value to the Swift mission by discovering and characterizing new millisecond pulsar binaries through ground-based correlative observations, including spider binaries that represent the most massive and fastest spinning neutron stars, transitional millisecond pulsars, and other rare systems that offer novel constraints on neutron star formation and evolution.
2124113 / AUCHETTL / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)
"SWIFT'S MULTI-WAVELENGTH VIEW OF THE NEXT NEARBY TDE"
Current optical surveys that are wider, deeper and have high temporal cadence are poised to find a number of TDEs before maximum light, granting us the opportunity to track the most crucial, yet currently missing, phase of their evolution. Probing the early phase of a TDE will advance our understanding of the emission mechanisms acting in these fascinating transients, which are linked to some of the most important astrophysical questions related to: black hole demographics, accretion disk formation and super-Eddington accretion. We propose to monitor 1 TDE discovered before peak with Swift. These data will place constraints on the early-time energetics of TDEs, which are critical for breaking the degeneracies in current TDE emission models as we continue to explore the TDE phase space.
2124115 / BORGHESE / OSSERVATORIO ASTRONOMICO DI ROMA
"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.
2124119 / FUERST / EUROPEAN SPACE ASTRONOMY CENTRE (ESAC)
"SWIFT MONITORING OF THE ULTRA-LUMINOUS X-RAY PULSAR NGC 7793 P13"
One of the most interesting ultra-luminous X-ray pulsars (ULXPs) is NGC 7793 P13, which stands out owing to its high duty cycle of pulsations, as well as being the only ULX pulsar where we know both the nature of the companion star and the full orbital ephemeris. Here we propose to continue the Swift monitoring program of P13, adding to the data taken in the last AOs and making full use of the combined power of the XRT and the UVOT. These observations will allow us to follow-up on the known X-ray and UV flux periods of the system and investigate the duty cycle of low- or off-states, one of which occurred between 2020-2021. They will also allow us to monitor other bright and transient X-ray sources in NGC 7793, like the black-hole candidate P9.
2124127 / 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 population of TDEs. 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.
2124131 / LANZ / THE COLLEGE OF NEW JERSEY
"AGN CHARACTERISTICS OF RECENTLY QUENCHED GALAXIES"
The necessity of feedback from AGN in galaxy evolution is clear based on multiple observational signatures, including galaxies and clusters showing AGN jets or outflows and correlations between galactic bulge mass and SMBH mass. The precise role played by AGN in quenching star formation and the conditions under which AGN are the primary cause of quenching remain unclear. One approach is to use galaxies with signatures of recent quenching and examine their characteristics, including AGN activity. To date, this has been done with small samples. We propose to use existing Swift X-ray observations to characterize AGN in recently quenched galaxies with counterparts in the 2SXPS using a forward-modeling approach to obtain individual constraints even in the presence of low-count detections.
2124135 / SIEGEL / THE PENNSYLVANIA STATE UNIVERSITY
"COMPLETING THE UV CENSUS OF GALACTIC GLOBULAR CLUSTERS"
Swift has obtained two- or three-band imaging of the bulk of Galactic globular clusters. This database is extremely useful for identifying rare bright stellar types, testing models of stellar evolution, studying the UV properties of RR Lyrae stars and constraining the integrated light properties of old stellar populations. These studies are especially useful when combined with existing GALEX imaging. However, there are a number of important clusters that have not been surveyed by UVOT. And surveys of very rare stellar types -- such as Above the Horizontal Branch (AHB) stars -- benefit from having a nearly-complete census. We propose to complete the Swift survey of globular clusters by obtaining three-band imaging of the 20 clusters remaining to be studied.
2124137 / GAUDIN / THE PENNSYLVANIA STATE UNIVERSITY
"DEEP MONITORING OF THE SMC BE/X-RAY BINARY POPULATION DURING LUMINOUS OUTBURST"
We propose follow-up Target of Opportunity (TOO) observations of Be/X-ray binary (BeXRB) systems in the Small Magellanic Cloud (SMC) during luminous outburst events. Requested observations will utilize both X-ray timing and spectral measurements as well as ultraviolet/optical photometry to monitor systems for a large fraction of their orbit. These measurements will be used to constrain the accretion mechanism driving the outburst, identify physical properties of the system such as the orbital parameters, and monitor the evolution of the circumstellar disk structure.
2124138 / DICHIARA / THE PENNSYLVANIA STATE UNIVERSITY
"SEARCHING HIGH AND LOW FOR ELUSIVE SHORT GRBS"
We propose a follow-up program dedicated to the search for the optical/nIR counterparts of short duration gamma-ray bursts (sGRBs) using our accepted programs on space-based and ground-based telescopes. We will use photometric and spectroscopic measurements to estimate the redshifts of these sGRBs, study their afterglows and identify any signatures of a radioactive-powered kilonova. The proposed work is critical for identifying the population of high redshift (z>1) sGRBs and rare nearby (z<0.1) events. It will greatly enhance the science return of Swift observations, and provide a vital complement to gravitational wave astronomy.
2124145 / 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.
2124146 / SOKOLOSKI / COLUMBIA UNIVERSITY
"MULTI-WAVELENGTH 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 21 or until T CrB erupts.
2124152 / RAJGURU / CLEMSON UNIVERSITY
"TRACING THE MOST POWERFUL JETS THROUGH COSMIC TIME"
For the very first time we have detected 6 new MeV blazars in the 20-200 MeV band that lack 2-10 keV data. These powerful MeV blazars, and other sources detected in our catalog, will pave the way to the exploration of the MeV sky in anticipation of COSI. We request to observe the 6 sources with Swift for a total of 101 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 s luminosity and the black hole mass.
2124154 / CHIRENTI / UNIVERSITY OF MARYLAND (COLLEGE PARK)
"A SEARCH FOR QUASIPERIODIC OSCILLATIONS IN SHORT GAMMA RAY BURSTS DETECTED BY SWIFT/BAT"
Short gamma-ray bursts (SGRBs) have been associated with binary neutron star mergers. The end result of such a merger can be a stable neutron star, a millisecond magnetar that collapses to a black hole or direct collapse to a black hole. The detection of quasiperiodic oscillations (QPOs) in SGRBs, recently achieved by a rigorous timing analysis within a Bayesian framework, could provide clues to the SGRB progenitor. High-frequency QPOs (> 1 kHz), reported in two BATSE SGRBs, are consistent with the millisecond magnetar remnant scenario. A low-frequency QPO (< 100 Hz), identified in a recent BAT GRB, is consistent e.g. with the precession of a protoneutron star or Lense-Thirring precession. Here we propose a thorough search for QPOs in the Swift catalog and current data.
2124156 / BODEWITS / AUBURN UNIVERSITY
"THE ACTIVITY AND EVOLUTION OF OORT CLOUD COMETS AT A WIDE RANGE OF DISTANCES"
We propose to use Swift UVOT to characterize the activity and evolution of the Oort cloud comets C/2023 A3 (Tsuchinshan-ATLAS) and C/2024 E1 (Wierzchos), which both become exceptionally bright even at large distances from the Sun and have remarkably small perihelion distances. We will use photometric imaging to measure production rates of OH (a direct proxy for water) and dust over the course of their apparitions. Swift s unique capabilities will allow us to monitor the onset, demise, and relative contributions of water released from different sources on the nucleus and in the coma as these comets are increasingly heated by the Sun. These observations will allow us to characterize the storage and release of cometary volatiles, which allows connecting them to planet formation models.
2124165 / MARCULEWICZ / WAYNE STATE UNIVERSITY
"WEAK EMISSION-LINE QUASARS IN THE UV - THE MISSING PIECE TO CONSTRAIN THE BLACK HOLE MASS"
Weak emission-line quasars (WLQs) are a peculiar subclass of Active Galactic Nuclei (AGN), that show show weak or absent emission lines. These objects remain poorly understood, but key to narrowing down models is determining whether they accrete at low or high rates. Critical to this is accurate black hole masses. But, their anomalous emission line properties mean that standard mass estimates from scaling relations are unreliable. Previous studies modeling broadband spectral energy distributions demonstrate potential for measure masses, but lacked good coverage in the UV where disk models are the most constraining. Here we propose a Swift survey of 9 WLQs with all six UVOT filters to significantly improve black hole mass estimates, and hence better understand the accretion flow in WLQs.
2124177 / VIELIUTE / UNIVERSITY OF ST. ANDREWS
"DISENTANGLING THE SPECTRAL ENERGY DISTRIBUTION OF AGN IN INTENSIVE GROUND-BASED MONITORING CAMPAIGNS"
The Spectral Energy Distribution (SED) of Active Galactic Nuclei (AGN) reveals critical information about accretion theory onto supermassive black holes, yet it is often contaminated by underlying emission from the host galaxy. The correlated variability at different energies (UV to optical) can be used to decompose the SED of the 'stationary' host galaxy and the 'variable' AGN, using contemporaneous Swift and ground-based observations. We propose to use Swift to extend the determination of the broadband SED of nine local AGN which will be target of intensive ground-based reverberation mapping campaigns. Swift will deliver monthly observations in the three UV filters and an average X-ray spectrum over the course of Cycle 21.
2124184 / 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 hundredsof times longer. Some are periodic on timescales of minutes to hours, and are broadly known as Ultra-Long Period objects (ULPs). Others show longer-lasting emission and may be part of the growing class of Galactic Center Radio Transients. 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.
2124185 / MOONEY / UNIVERSITY OF DELAWARE
"INVESTIGATING THE X-RAY AND TEV CORRELATION OF VER J0521+211 WITH SWIFT-XRT AND VERITAS"
The correlation between X-ray and TeV fluxes in blazars like Mrk 421 hints at a single, confined particle acceleration zone for both emissions. This relationship, tighter than expected, underscores the need to investigate the underlying mechanisms. Our proposal focuses on VER J0521+211, a high-energy blazar with a significant gamma-ray luminosity, about ten times larger than that of Mrk 421 and Mrk 501. This implies a larger jet power and potentially more complex system. To explore this, we propose a monitoring campaign with Swift-XRT and VERITAS, aiming to quantify the synchrotron and inverse-Compton emissions' correlation with simultaneous observations. This data will help us understand electron acceleration and cooling dynamics, particularly with multiple soft photon populations
2124187 / SAND / UNIVERSITY OF ARIZONA
"UV IMAGING OF NEWLY DISCOVERED DWARF GALAXIES IN THE VERY NEARBY UNIVERSE"
We request Swift UV imaging of 22 newly discovered, low mass dwarf galaxies which have no pre-existing UV data, part of a larger sample identified with a novel CNN technique. The hallmark of this sample is that most new dwarfs are in an `isolated' environment far from any massive galaxy, and so have never been subjected to the altering affects of ram pressure stripping, allowing us to probe the role that reionization and internal feedback play in the smallest galaxies. UV observations are sensitive to the star formation rate within the last 100 Myr, which may be truncated or sporadic due to the above processes. Only by building a comprehensive sample with multi-wavelength data can these affects be traced as a function of dwarf galaxy stellar mass, star formation rate and gas content.
2124192 / 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. We aim to follow up to two neutrinos with energy above 100 TeV that will be detected by KM3NeT in the observation period
2124198 / MCBRIDE / BOWDOIN COLLEGE
"X-RAY SIGNATURES OF NEUTRINO EMITTERS"
Swift follow-up observations of an high-energy neutrino provided the first compelling evidence of an extragalactic neutrino source, the flaring blazar TXS 0506+056. We propose prompt X-ray and UV/optical follow-up observations of IceCube-detected neutrinos. For well-localized track events, we will use a 7-pointing XRT mosaic with 500s exposures, totaling 3.5ks per event. If a promising source is identified, we will conduct an additional 1ks observation. For less localized events, we will target up to 7 candidate sources within the uncertainty region. In total, we request 28.5ks of Swift observing time. Identifying high-energy neutrino sources is crucial for understanding neutrino and cosmic-ray production mechanisms and could reveal new source populations or the origins of the cosmic rays.
2124203 / 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 radiation simultaneously powers PAH emission (which dominates the mid-infrared), whilst also processing and destroying PAHs. PAH abundance is also hugely metallicity-dependent. JWST recently targeted PAH emission in 6 regions in M101 spanning 0.93 dex in metallicity. UVOT is uniquely suited to constraining the hardness and intensity of the UV radiation field, vital for interpreting PAH emission. 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 sky coverage around M101 caus.
2124205 / HOSSEINZADEH / 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.
2124207 / HAMMERSTEIN / UNIVERSITY OF CALIFORNIA (BERKELEY)
"STELLAR DESTRUCTION ON THE RISE: INFANT TIDAL DISRUPTION EVENTS WITH SWIFT"
Over the last decade there has been major progress in the search for tidal disruption events (TDEs) in wide-field surveys across the electromagnetic spectrum, particularly in the optical. However, the origin of this optical emission remains a mystery. Here we propose a Swift Cycle 21 program to confirm and monitor a sample of optically-selected TDEs in their infancy within a week of optical discovery (or first optical detection). These observations will be able to test the viability of models for the optical emission in TDEs, a crucial goal if we hope to unlock the full power of TDEs as probes of supermassive black holes (SMBHs) in future time-domain surveys.
2124211 / LIN / NORTHEASTERN UNIVERSITY
"TWO UNIQUE SOURCES IN A ROW: ESO 243-49 HLX-1 AND A NEWBORN HARD TIDAL DISRUPTION EVENT"
In Neil Gehrels Swift Observatory GI Cycle 21, we propose 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 explore the system's ultimate fate, including potential donor star ejection. For the hard TDE, we seek to detect new giant, fast X-ray flares and to identify recurrent outbursts, an intriguing feature in multiple TDEs of similar spectral properties.
2124212 / LAWTHER / UNIVERSITY OF ARIZONA
"CAPTURING THE BRIGHT STATE OF A RE-IGNITED AGN"
Mrk 590 is a changing-look AGN (CLAGN) that fully re-ignited during the first half of 2024, after several years of X-ray--driven flaring. We ask to monitor Mrk 590 with Swift every four days. In concert with ground-based UV--optical spectroscopic monitoring, and ToO observations with HST, we will measure the size and ionization stratification of the broad-line region. By characterizing the optical--UV--X-ray SED and its variability, we will determine the nature of the ionizing continuum source in this new bright state. Via an in-depth comparison with existing observations in the most recent `turn-off' state (late 2023), we will test models for CLAGN activity where the disk is passive or truncated at lower luminosities, leading to a lack of ionizing photons for broad line production.
2124218 / WALSH / NIELS BOHR INSTITUTE
"SWIFT AND THE VLBA UNMASK THE CHANGING-LOOK AGN MRK 590"
Mrk 590 is dramatic even among the changing-look AGN (CLAGN) population and has recently exhibited behavior indicative of a state change of its accretion flow. Despite nearly a decade of radio monitoring, the progenitor of the low-luminosity radio emission from Mrk 590 remains an enigma. Now, as the AGN transitions between accretion states, we have the ability to not only directly constrain the radio emission progenitor but also explore the interdependence of accretion-driven (optical/UV/X-ray) and radio emission phenomena at the highest mass scale. This joint Swift-VLBA program will, for the first time, test if state transitions of the accretion flow in CLAGN directly affect the AGN s ability to launch a collimated radio jet and examine the physical parameters driving radio variability.
2124237 / SANTANDER / UNIVERSITY OF ALABAMA
"PINPOINTING THE SOURCES OF THE ISOTROPIC GAMMA-RAY BACKGROUND WITH SWIFT"
The origin of the diffuse isotropic gamma-ray background measured by the Fermi gamma-ray satellite at energies between 100 MeV and 820 GeV remains largely uncertain. Population studies indicate that most of the emission originates in a large number of extragalactic objects such as active galactic nuclei, star-forming galaxies, or radio galaxies too faint to be resolved as individual sources. We here propose a ToO program aimed at pinpointing AGN counterparts to VHE Fermi-LAT photons and therefore help constrain the composition of the IGRB at energies above 250 GeV.
2124240 / WARD / PRINCETON UNIVERSITY
"EXPLORING THE PHYSICAL ORIGIN OF COMPACT MILLIMETER EMISSION IN RADIO-QUIET AGN WITH SWIFT X-RAY MONITORING"
Time-domain surveys at millimeter and radio wavelengths are probing new physics for new populations of AGN and nuclear transients. This provides us with an exciting opportunity to study the origin of mm emission in radio-quiet AGN, providing insights into open questions about a potentially common coronal origin for radio, mm, and X-ray emission in these objects. We request monthly cadence Swift monitoring of two radio-quiet AGN that will have simultaneous mm and radio monitoring by the SPT and ASKAP VAST surveys. By identifying multi-wavelength variability correlations, we will learn much about the physics of coronal emission and compact radio jets in this AGN subclass, and enable larger population studies with the next generation of mm and radio surveys.
2124242 / DURBAK / UNIVERSITY OF MARYLAND (COLLEGE PARK)
"RIMAS - RAPID INFRARED IMAGER-SPECTROMETER A FACILITY FOR A FAST FOLLOWUP ON HIGH REDSHIFT GRBS"
RIMAS is a new NIR instrument designed expressly to identify high-redshift GRBs from Swift, scheduled to be installed on the 4.3 m LDT during the Fall 2024 semester. 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 21, 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 galaxy and surrounding IGM.
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