Swift Cycle 18 Results

The lists below contain the proposals recommended by the Cycle 18 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 18 proposals for observation: Please note that the ROSES 2020 Appendix D.5 "Swift Guest Investigator Cycle 18" 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 five hours in RA from the Sun and more than 20 degrees from the Moon before requesting Swift observations (http://heasarc.gsfc.nasa.gov/Tools/Viewing.html).

Accepted Cycle 18 ToO proposals may be triggered until March 31, 2023"."

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.

Recommended Proposals

Prop        PI                  Title
1821006     KENNEA              RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS IN CYCLE 18
1821015     KENNEA              KEY PROJECT: THE DETECTION AND MONITORING OF ELECTROMAGNETIC COUNTERPARTS OF GRAVITATIONAL
                                WAVE SOURCES WITH SWIFT IN O4
1821023     MASETTI             SWIFT SNAPSHOT SURVEY OF SUSPECT SYMBIOTIC STARS IN THE GALAH ARCHIVE (S^6-GALAH)
1821026     BOGDANOV            SWIFT MONITORING OF NEARBY X-RAY BINARY-RADIO MILLISECOND PULSAR TRANSITION OBJECTS
1821027     MARSCHER            COMBINED SWIFT AND IXPE OBSERVATIONS OF BLAZARS
1821033     AUCHETTL            PROBING THE EARLY UV AND X-RAY EVOLUTION OF TDES
1821035     AUCHETTL            BRIGHT OPTICAL TDES AND THEIR FINAL STAGES OF EVOLUTION
1821042     SHENG               PHOTOMETRIC REDSHIFTS FOR FERMI BLAZARS WITH SWIFT/UVOT
1821052     TORRES-ALBA         THE LEGACY OF SWIFT-BAT: THE HARD X-RAY SKY
1821055     DEGENAAR            A SWIFT LEGACY: THE MONITORING CAMPAIGN OF THE GALACTIC CENTER
1821061     HOWARD              A SWIFT AND ALMA VIEW OF THE ORIGIN AND IMPACT OF M-DWARF FLARES
1821065     MACCARONE           THE SWIFT GALACTIC BULGE MONITORING SURVEY: FOURTH EPOCH
1821074     KAUR                EXPLORING UNPROBED X-RAY VARIABILITY IN M87 DURING THE 2022 EVENT HORIZON TELESCOPE (EHT)
                                MULTIWAVELENGTH CAMPAIGN USING
1821075     MARGUTTI            A SWIFT INVESTIGATION OF FAST BLUE OPTICAL TRANSIENTS
1821087     GELBORD             EXTENDED MONITORING OF THE DRAMATICALLY-VARYING AGN MRK 817
1821088     HOMAN               OBSERVING THE EARLY RISE OF X-RAY TRANSIENTS WITH SWIFT
1821090     VAN DEN EIJNDEN     SWIFT/VLA MONITORING OF THE DECAY OF A GIANT BE/X-RAY BINARY OUTBURST
1821092     OATES               LATE TIME UV OBSERVATIONS OF J221951-484240: AN UNUSUAL TDE OR AGN
1821098     SOKOLOVSKY          IN SEARCH OF SHOCKS IN NOVAE
1821101     KRUMPE              SWIFT FOLLOW-UP OF RARE AGN IGNITION AND SHUT-DOWN EVENTS DETECTED WITH EROSITA
1821102     MILLER              ABSOLUTE ULTRAVIOLET PHOTOMETRY OF ECLIPSING BINARY STARS
1821108     CORSI               A SEARCH FOR BL-IC SNE WITH X-RAY AFTERGLOWS USING ZTF+SWIFT
1821110     CHELOUCHE           SHEDDING LIGHT ON LIGHT ECHOES: MAPPING THE CONTINUUM EMITTING REGIONS IN MRK 279 USING
                                SWIFT AND HST
1821125     WALTON              TESTING THE LENSE-THIRRING MODEL FOR ULX VARIABILITY WITH NGC5907 ULX1
1821134     LAWTHER             CAPTURING THE RE-IGNITION OF THE BROAD LINE REGION IN MRK 590
1821142     SIEGEL              A SWIFT/UVOT STUDY OF RR LYRAE IN M62 AND M5
1821143     JACKMAN             UNDERSTANDING THE DISCONNECT BETWEEN NUV AND WHITE-LIGHT FLARE EMISSION FROM LOW-MASS
                                STARS WITH CR DRA
1821150     SANTANDER           PINGING DOWN NEUTRINO-BLAZAR EMITTERS WITH SWIFT
1821153     PASHAM              TRACKING THE LONG-TERM EVOLUTION OF QUASI-PERIODIC ERUPTIONS FROM THE NUCLEUS OF A PASSIVE
                                GALAXY USING XRT MONITORING
1821154     SHAW                BLACK HOLE JET LAUNCHING PHYSICS: TRIGGERING JWST WITH SWIFT
1821158     JACKMAN             DO OPTICALLY QUIET M STARS SHOUT IN THE NUV?
1821161     NICOTRA             CLOSING IN ON THE PROGENITORS OF FAST RADIO BURSTS
1821162     BROWN               NOT DONE YET: TEMPLATE OBSERVATIONS TO COMPLETE
1821168     PENIL               SWIFT CHARACTERIZATION OF PERIODIC-EMISSION BLAZARS
1821171     BODEWITS            WHY WAS COMET C/2017 K2 ACTIVE AT RECORD-SETTING DISTANCES AND WHAT HAPPENS WHEN IT REACHES
                                THE INNER SOLAR SYSTEM?
1821172     FOLEY               EXTREMELY YOUNG TRANSIENTS
1821173     HOMAN               INVESTIGATING SHALLOW HEATING IN NEUTRON STAR CRUSTS
1821174     LAHA                CAUGHT IN THE ACT: A SWIFT TOO CAMPAIGN ON CHANGING-LOOK AGN
1821190     MCHARDY             THE X-RAY/RADIO LINK IN RADIO-QUIET AGN
1821191     PASHAM              CAPTURING QUASI-PERIODIC OUTFLOWS FROM A FUTURE AGN OUTBURST USING XRT AND UVOT MONITORING
1821197     GOTTLIEB            SEARCHING HIGH AND LOW FOR ELUSIVE SHORT GRBS
1821199     FOLEY               PROBING THE PROGENITOR METALLICITY OF TYPE IA SUPERNOVAE WITH EARLY-TIME UV SPECTROSCOPY
1821203     LIN                 TWO UNIQUE SOURCES IN A ROW: ESO 243-49 HLX-1 AND A NEWBORN HARD TIDAL DISRUPTION EVENT
1821204     DONG                HIGH-CADENCE UV LIGHT CURVES OF EXTREMELY YOUNG SUPERNOVAE

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 ] |

1821006 | KENNEA          | 1          | FRB #1              | 2           | Y   | 0          | 0           |
1821006 | KENNEA          | 2          | FRB #2              | 2           | Y   | 0          | 0           |
1821006 | KENNEA          | 3          | FRB #3              | 2           | Y   | 0          | 0           |
1821006 | KENNEA          | 4          | FRB #4              | 2           | Y   | 0          | 0           |
1821006 | KENNEA          | 5          | FRB #5              | 2           | Y   | 0          | 0           |
1821006 | KENNEA          | 6          | FRB #6              | 2           | Y   | 0          | 0           |
1821006 | KENNEA          | 7          | FRB #7              | 2           | Y   | 0          | 0           |
1821006 | KENNEA          | 8          | FRB #8              | 2           | Y   | 0          | 0           |
1821006 | KENNEA          | 9          | FRB #9              | 2           | Y   | 0          | 0           |
1821006 | KENNEA          | 10         | FRB #10             | 2           | Y   | 0          | 0           |
1821015 | KENNEA          | 1          | GW EM CANDIDATE #1  | 70          | Y   | 0.01       | 0           |
1821015 | KENNEA          | 2          | GW EM CANDIDATE #2  | 70          | Y   | 0.01       | 0           |
1821015 | KENNEA          | 3          | GW EM CANDIDATE #3  | 70          | Y   | 0.01       | 0           |
1821023 | MASETTI         | 1          | A2-006              | 1           | N   | 59.58821   | 22.81281    |
1821023 | MASETTI         | 2          | A2-010              | 1           | N   | 67.15696   | 1.90417     |
1821023 | MASETTI         | 3          | A2-011              | 1           | N   | 68.59775   | -7.54333    |
1821023 | MASETTI         | 4          | A2-030              | 1           | N   | 81.60679   | 5.31308     |
1821023 | MASETTI         | 5          | A2-046              | 1           | N   | 124.25533  | -15.66917   |
1821023 | MASETTI         | 6          | A2-054              | 1           | N   | 127.35162  | -21.40547   |
1821023 | MASETTI         | 7          | A2-077              | 1           | N   | 167.96371  | -0.34986    |
1821023 | MASETTI         | 8          | A2-103              | 1           | N   | 231.84725  | -6.31089    |
1821023 | MASETTI         | 9          | A2-106              | 1           | N   | 233.31     | -16.81478   |
1821023 | MASETTI         | 10         | A2-117              | 1           | N   | 235.76008  | -19.98108   |
1821023 | MASETTI         | 11         | A2-122              | 1           | N   | 236.58496  | -20.12525   |
1821023 | MASETTI         | 12         | A2-129              | 1           | N   | 239.283    | -26.28869   |
1821023 | MASETTI         | 13         | A2-145              | 1           | N   | 242.11113  | -22.93175   |
1821023 | MASETTI         | 14         | A2-147              | 1           | N   | 242.28104  | -21.97208   |
1821023 | MASETTI         | 15         | A2-151              | 1           | N   | 242.42604  | -17.44306   |
1821023 | MASETTI         | 16         | A2-160              | 1           | N   | 243.24804  | -19.28989   |
1821023 | MASETTI         | 17         | A2-164              | 1           | N   | 243.566    | -27.7555    |
1821023 | MASETTI         | 18         | A2-171              | 1           | N   | 245.4165   | -16.59825   |
1821023 | MASETTI         | 19         | A2-173              | 1           | N   | 245.77842  | -17.19211   |
1821023 | MASETTI         | 20         | A2-178              | 1           | N   | 246.55271  | 6.38897     |
1821023 | MASETTI         | 21         | A2-206              | 1           | N   | 249.55254  | -28.14083   |
1821023 | MASETTI         | 22         | A2-207              | 1           | N   | 249.76417  | -19.75369   |
1821023 | MASETTI         | 23         | A2-222              | 1           | N   | 256.26587  | -20.66525   |
1821023 | MASETTI         | 24         | A2-224              | 1           | N   | 256.87175  | -17.87344   |
1821023 | MASETTI         | 25         | A2-231              | 1           | N   | 259.35875  | -17.41419   |
1821023 | MASETTI         | 26         | A2-234              | 1           | N   | 264.19825  | -8.28897    |
1821023 | MASETTI         | 27         | A2-235              | 1           | N   | 265.56696  | -16.03072   |
1821023 | MASETTI         | 28         | A2-236              | 1           | N   | 266.03838  | 5.74953     |
1821023 | MASETTI         | 29         | A2-255              | 1           | N   | 280.86342  | -28.56242   |
1821023 | MASETTI         | 30         | A2-256              | 1           | N   | 281.21058  | -22.75361   |
1821023 | MASETTI         | 31         | A2-276              | 1           | N   | 282.51862  | -24.90056   |
1821023 | MASETTI         | 32         | A2-287              | 1           | N   | 284.63396  | -26.47578   |
1821023 | MASETTI         | 33         | A2-289              | 1           | N   | 285.06679  | -23.83264   |
1821023 | MASETTI         | 34         | A2-292              | 1           | N   | 285.36875  | -26.80594   |
1821023 | MASETTI         | 35         | A2-297              | 1           | N   | 286.0695   | -15.71469   |
1821023 | MASETTI         | 36         | A2-303              | 1           | N   | 287.60383  | -20.66311   |
1821023 | MASETTI         | 37         | A2-323              | 1           | N   | 289.97454  | -15.75633   |
1821023 | MASETTI         | 38         | A2-336              | 1           | N   | 292.22492  | -28.44558   |
1821023 | MASETTI         | 39         | A2-344              | 1           | N   | 298.12183  | 3.45372     |
1821023 | MASETTI         | 40         | A2-354              | 1           | N   | 302.44083  | 0.86464     |
1821026 | BOGDANOV        | 1          | PSR J1023+0038      | 4           | N   | 155.94871  | 0.64475     |
1821026 | BOGDANOV        | 2          | XSS J12270-4859     | 4           | N   | 186.99475  | -48.89522   |
1821026 | BOGDANOV        | 3          | PSR J1723-2837      | 4           | N   | 260.84658  | -28.63253   |
1821026 | BOGDANOV        | 4          | PSR J1628-3205      | 4           | N   | 247.02925  | -32.09686   |
1821026 | BOGDANOV        | 5          | PSR J2129-0429      | 4           | N   | 322.4375   | -4.48489    |
1821026 | BOGDANOV        | 6          | PSR J1816+4510      | 4           | N   | 274.14971  | 45.17608    |
1821026 | BOGDANOV        | 7          | PSR J2215+5135      | 4           | N   | 333.88617  | 51.59347    |
1821026 | BOGDANOV        | 8          | PSR J2339-0533      | 4           | N   | 354.91146  | -5.55147    |
1821026 | BOGDANOV        | 9          | 1FGL J0523.5-2529   | 4           | N   | 80.8205    | -25.46025   |
1821026 | BOGDANOV        | 10         | PSR J1417-4402      | 4           | N   | 214.3775   | -44.04925   |
1821026 | BOGDANOV        | 11         | 3FGL J1544.6-1125   | 4           | N   | 236.16408  | -11.46786   |
1821026 | BOGDANOV        | 12         | 3FGL J0427.9-6704   | 4           | N   | 66.95671   | -67.07639   |
1821026 | BOGDANOV        | 13         | PSR J1048+2339      | 4           | N   | 162.18088  | 23.66483    |
1821026 | BOGDANOV        | 14         | 3FGL J0212.1+5320   | 4           | N   | 33.04358   | 53.336      |
1821026 | BOGDANOV        | 15         | 3FGL J0744.1-2523   | 4           | N   | 116.03529  | -25.39969   |
1821026 | BOGDANOV        | 16         | 3FGL J0838.8-2829   | 4           | N   | 129.71021  | -28.46594   |
1821026 | BOGDANOV        | 17         | 3FGL J2039.6-5618   | 4           | N   | 309.89579  | -56.28583   |
1821027 | MARSCHER        | 1          | MKN421              | 54          | N   | 166.11379  | 38.20883    |
1821027 | MARSCHER        | 2          | MKN501              | 63          | N   | 253.46758  | 39.76017    |
1821027 | MARSCHER        | 3          | CEN A               | 18          | N   | 201.36508  | -43.01911   |
1821027 | MARSCHER        | 4          | 1ES1959+65          | 45          | N   | 299.99942  | 65.1485     |
1821027 | MARSCHER        | 5          | 3C454.3             | 6           | N   | 343.49062  | 16.14822    |
1821027 | MARSCHER        | 6          | 3C454.3             | 18          | N   | 343.49062  | 16.14822    |
1821027 | MARSCHER        | 7          | 3C279               | 6           | N   | 194.04654  | -5.78931    |
1821027 | MARSCHER        | 8          | 3C279               | 18          | N   | 194.04654  | -5.78931    |
1821027 | MARSCHER        | 9          | BLLAC               | 6           | N   | 339.68038  | 42.27778    |
1821027 | MARSCHER        | 10         | BLLAC               | 18          | N   | 339.68038  | 42.27778    |
1821027 | MARSCHER        | 11         | J0211+1051          | 3           | N   | 32.80492   | 10.85967    |
1821027 | MARSCHER        | 12         | J0211+1051          | 9           | N   | 32.80492   | 10.85967    |
1821027 | MARSCHER        | 13         | 0716+714            | 3           | N   | 110.47271  | 71.34339    |
1821027 | MARSCHER        | 14         | 0716+714            | 9           | N   | 110.47271  | 71.34339    |
1821027 | MARSCHER        | 15         | 1ES0229+20          | 3           | N   | 38.20258   | 20.28819    |
1821027 | MARSCHER        | 16         | 1ES0229+20          | 9           | N   | 38.20258   | 20.28819    |
1821027 | MARSCHER        | 17         | PKS2155-30          | 3           | N   | 329.71696  | -30.22558   |
1821027 | MARSCHER        | 18         | PKS2155-30          | 9           | N   | 329.71696  | -30.22558   |
1821033 | AUCHETTL        | 1          | BH-TDE              | 62          | Y   | 0          | 0           |
1821035 | AUCHETTL        | 1          | ASASSN-14LI         | 6           | N   | 192.06333  | 17.774      |
1821035 | AUCHETTL        | 2          | ASASSN-14AE         | 5           | N   | 167.16717  | 34.09783    |
1821035 | AUCHETTL        | 3          | ASASSN-15OI         | 6           | N   | 309.78825  | -30.75558   |
1821035 | AUCHETTL        | 4          | IPTF16FNL           | 5           | N   | 7.48754    | 32.89367    |
1821035 | AUCHETTL        | 5          | AT2018DYB           | 5           | N   | 242.74487  | -60.92311   |
1821035 | AUCHETTL        | 6          | ASASSN-18ZJ         | 4           | N   | 151.71196  | 1.69281     |
1821035 | AUCHETTL        | 7          | ASASSN-19BT         | 6           | N   | 105.04812  | -66.04003   |
1821035 | AUCHETTL        | 8          | ASASSN-19DJ         | 6           | N   | 123.32058  | 22.64833    |
1821035 | AUCHETTL        | 9          | AT2019DSG           | 4           | N   | 314.26237  | 14.20442    |
1821035 | AUCHETTL        | 10         | AT2019QIZ           | 4           | N   | 71.65783   | -10.22636   |
1821035 | AUCHETTL        | 11         | AT2020NEH           | 5           | N   | 230.33371  | 14.06958    |
1821035 | AUCHETTL        | 12         | AT2020NOV           | 6           | N   | 254.55404  | 2.1175      |
1821035 | AUCHETTL        | 13         | AT2020VWL           | 6           | N   | 232.6575   | 26.98247    |
1821035 | AUCHETTL        | 14         | AT2021BLZ           | 6           | N   | 68.13021   | -32.43064   |
1821035 | AUCHETTL        | 15         | AT2021KQP           | 5           | N   | 223.79475  | -6.98589    |
1821042 | SHENG           | 1          | 3FGL J0836.3+2143   | 2           | N   | 129.06758  | 21.651      |
1821042 | SHENG           | 2          | 3FGL J1218.5+6912   | 2           | N   | 185.18567  | 69.09036    |
1821042 | SHENG           | 3          | 3FGL J1138.2+4905   | 2           | N   | 174.50862  | 48.98244    |
1821042 | SHENG           | 4          | 3FGL J0133.2-5159   | 2           | N   | 23.274     | -52.00108   |
1821042 | SHENG           | 5          | 3FGL J0928.7+7300   | 2           | N   | 142.25017  | 72.95286    |
1821042 | SHENG           | 6          | 3FGL J0218.9+3642   | 2           | N   | 34.7085    | 36.6785     |
1821042 | SHENG           | 7          | 3FGL J1331.5+1711   | 2           | N   | 202.88933  | 17.21406    |
1821042 | SHENG           | 8          | 3FGL J2235.6-2319   | 2           | N   | 339.10933  | -23.15739   |
1821042 | SHENG           | 9          | 3FGL J0301.8-7157   | 2           | N   | 45.41021   | -71.94289   |
1821042 | SHENG           | 10         | 3FGL J1516.9+1926   | 2           | N   | 229.23667  | 19.53694    |
1821042 | SHENG           | 11         | 3FGL J1840.5+6116   | 2           | N   | 280.14829  | 61.23497    |
1821042 | SHENG           | 12         | 3FGL J1723.5-5609   | 2           | N   | 260.93571  | -56.24822   |
1821042 | SHENG           | 13         | 3FGL J1500.6+4750   | 2           | N   | 225.20271  | 47.85431    |
1821042 | SHENG           | 14         | 3FGL J0846.7-0651   | 2           | N   | 131.98642  | -7.05469    |
1821042 | SHENG           | 15         | 3FGL J0638.4+5704   | 2           | N   | 99.60758   | 57.03056    |
1821042 | SHENG           | 16         | 3FGL J0707.2+6101   | 2           | N   | 106.75237  | 61.16961    |
1821042 | SHENG           | 17         | 3FGL J1704.0+7646   | 2           | N   | 255.99117  | 76.76947    |
1821042 | SHENG           | 18         | 3FGL J2212.3-7039   | 2           | N   | 332.98429  | -70.65411   |
1821042 | SHENG           | 19         | 3FGL J1035.2+5545   | 2           | N   | 158.93979  | 55.71514    |
1821042 | SHENG           | 20         | 3FGL J0928.5+4048   | 2           | N   | 142.15567  | 40.812      |
1821052 | TORRES-ALBA     | 1          | PBC_NEW_027         | 2           | N   | 289.30717  | -28.58964   |
1821052 | TORRES-ALBA     | 2          | PBC_NEW_040         | 2           | N   | 329.79542  | -54.88939   |
1821052 | TORRES-ALBA     | 3          | PBC_NEW_043         | 2           | N   | 79.82492   | 17.71442    |
1821052 | TORRES-ALBA     | 4          | PBC_NEW_044         | 2           | N   | 290.45567  | -58.92931   |
1821052 | TORRES-ALBA     | 5          | PBC_NEW_045         | 2           | N   | 14.96354   | 39.19539    |
1821052 | TORRES-ALBA     | 6          | PBC_NEW_049         | 2           | N   | 52.26596   | 40.7735     |
1821052 | TORRES-ALBA     | 7          | PBC_NEW_050         | 2           | N   | 344.47142  | 26.15119    |
1821052 | TORRES-ALBA     | 8          | PBC_NEW_051         | 2           | N   | 12.97542   | 44.29508    |
1821052 | TORRES-ALBA     | 9          | PBC_NEW_061         | 2           | N   | 110.93171  | -56.147     |
1821052 | TORRES-ALBA     | 10         | PBC_NEW_064         | 2           | N   | 193.0185   | 35.33897    |
1821052 | TORRES-ALBA     | 11         | PBC_NEW_065         | 2           | N   | 274.46496  | 47.27339    |
1821052 | TORRES-ALBA     | 12         | PBC_NEW_066         | 2           | N   | 244.10675  | -10.51236   |
1821052 | TORRES-ALBA     | 13         | PBC_NEW_126         | 2           | N   | 314.08079  | -32.25444   |
1821052 | TORRES-ALBA     | 14         | PBC_NEW_127         | 2           | N   | 86.55221   | -45.29353   |
1821052 | TORRES-ALBA     | 15         | PBC_NEW_132         | 2           | N   | 50.83342   | -36.54983   |
1821052 | TORRES-ALBA     | 16         | PBC_NEW_134         | 2           | N   | 203.5385   | -38.4595    |
1821052 | TORRES-ALBA     | 17         | PBC_NEW_136         | 2           | N   | 208.05329  | -49.11236   |
1821052 | TORRES-ALBA     | 18         | PBC_NEW_137         | 2           | N   | 344.19221  | -4.15339    |
1821052 | TORRES-ALBA     | 19         | PBC_NEW_138         | 2           | N   | 269.24779  | -45.32558   |
1821052 | TORRES-ALBA     | 20         | PBC_NEW_140         | 2           | N   | 171.37192  | -39.06981   |
1821052 | TORRES-ALBA     | 21         | PBC_NEW_143         | 2           | N   | 29.02583   | -50.46886   |
1821052 | TORRES-ALBA     | 22         | PBC_NEW_145         | 2           | N   | 313.67596  | -47.13578   |
1821052 | TORRES-ALBA     | 23         | PBC_NEW_151         | 2           | N   | 317.62958  | -52.54992   |
1821052 | TORRES-ALBA     | 24         | PBC_NEW_153         | 2           | N   | 9.97513    | -15.88375   |
1821052 | TORRES-ALBA     | 25         | PBC_NEW_154         | 2           | N   | 355.94046  | -72.11636   |
1821052 | TORRES-ALBA     | 26         | PBC_NEW_157         | 2           | N   | 18.826     | -38.11992   |
1821052 | TORRES-ALBA     | 27         | PBC_NEW_161         | 2           | N   | 282.012    | -29.89744   |
1821052 | TORRES-ALBA     | 28         | PBC_NEW_165         | 2           | N   | 335.85292  | -46.6065    |
1821052 | TORRES-ALBA     | 29         | PBC_NEW_166         | 2           | N   | 1.86279    | -41.36697   |
1821052 | TORRES-ALBA     | 30         | PBC_NEW_169         | 2           | N   | 213.19725  | 26.20081    |
1821052 | TORRES-ALBA     | 31         | PBC_NEW_171         | 2           | N   | 210.15887  | 64.30153    |
1821052 | TORRES-ALBA     | 32         | PBC_NEW_172         | 2           | N   | 271.03871  | -63.65914   |
1821052 | TORRES-ALBA     | 33         | PBC_NEW_174         | 2           | N   | 187.74004  | 47.20128    |
1821052 | TORRES-ALBA     | 34         | PBC_NEW_175         | 2           | N   | 297.31179  | 48.82389    |
1821052 | TORRES-ALBA     | 35         | PBC_NEW_176         | 2           | N   | 59.60167   | -5.56756    |
1821052 | TORRES-ALBA     | 36         | PBC_NEW_178         | 2           | N   | 346.60179  | 28.84083    |
1821052 | TORRES-ALBA     | 37         | PBC_NEW_183         | 2           | N   | 352.25379  | -35.18142   |
1821052 | TORRES-ALBA     | 38         | PBC_NEW_186         | 2           | N   | 246.65683  | -33.14822   |
1821052 | TORRES-ALBA     | 39         | PBC_NEW_187         | 2           | N   | 139.60054  | -12.95503   |
1821052 | TORRES-ALBA     | 40         | PBC_NEW_189         | 2           | N   | 55.44283   | -29.11258   |
1821052 | TORRES-ALBA     | 41         | PBC_NEW_192         | 2           | N   | 283.11158  | -57.58558   |
1821052 | TORRES-ALBA     | 42         | PBC_NEW_193         | 2           | N   | 208.9425   | -29.33181   |
1821052 | TORRES-ALBA     | 43         | PBC_NEW_194         | 2           | N   | 130.82821  | -70.42119   |
1821052 | TORRES-ALBA     | 44         | PBC_NEW_195         | 2           | N   | 35.81354   | -17.73139   |
1821052 | TORRES-ALBA     | 45         | PBC_NEW_198         | 2           | N   | 29.12079   | -20.65314   |
1821052 | TORRES-ALBA     | 46         | PBC_NEW_199         | 2           | N   | 320.84675  | 29.69486    |
1821052 | TORRES-ALBA     | 47         | PBC_NEW_200         | 2           | N   | 275.35208  | -54.8575    |
1821052 | TORRES-ALBA     | 48         | PBC_NEW_201         | 2           | N   | 268.65392  | 75.09481    |
1821052 | TORRES-ALBA     | 49         | PBC_NEW_205         | 2           | N   | 71.85575   | -52.35125   |
1821052 | TORRES-ALBA     | 50         | PBC_NEW_207         | 2           | N   | 164.49179  | 50.12667    |
1821052 | TORRES-ALBA     | 51         | PBC_NEW_208         | 2           | N   | 114.57642  | 36.08128    |
1821052 | TORRES-ALBA     | 52         | PBC_NEW_209         | 2           | N   | 264.48671  | 17.85397    |
1821052 | TORRES-ALBA     | 53         | PBC_NEW_212         | 2           | N   | 223.18488  | -13.27644   |
1821052 | TORRES-ALBA     | 54         | PBC_NEW_215         | 2           | N   | 356.04304  | 11.73706    |
1821052 | TORRES-ALBA     | 55         | PBC_NEW_216         | 2           | N   | 353.496    | 12.12567    |
1821052 | TORRES-ALBA     | 56         | PBC_NEW_217         | 2           | N   | 39.72608   | 14.06911    |
1821052 | TORRES-ALBA     | 57         | PBC_NEW_218         | 2           | N   | 166.68696  | -5.65983    |
1821052 | TORRES-ALBA     | 58         | PBC_NEW_219         | 2           | N   | 224.59233  | 20.3        |
1821052 | TORRES-ALBA     | 59         | PBC_NEW_220         | 2           | N   | 25.12642   | -15.47025   |
1821052 | TORRES-ALBA     | 60         | PBC_NEW_221         | 2           | N   | 275.29975  | 76.96386    |
1821052 | TORRES-ALBA     | 61         | PBC_NEW_222         | 2           | N   | 7.61287    | -53.06328   |
1821052 | TORRES-ALBA     | 62         | PBC_NEW_223         | 2           | N   | 346.04096  | 44.07189    |
1821052 | TORRES-ALBA     | 63         | PBC_NEW_225         | 2           | N   | 173.70617  | 30.65261    |
1821052 | TORRES-ALBA     | 64         | PBC_NEW_226         | 2           | N   | 196.20304  | -19.03306   |
1821052 | TORRES-ALBA     | 65         | PBC_NEW_228         | 2           | N   | 296.19633  | -46.37956   |
1821052 | TORRES-ALBA     | 66         | PBC_NEW_229         | 2           | N   | 124.51625  | 35.27036    |
1821052 | TORRES-ALBA     | 67         | PBC_NEW_230         | 2           | N   | 67.69187   | 28.05861    |
1821052 | TORRES-ALBA     | 68         | PBC_NEW_237         | 2           | N   | 300.78442  | -22.44078   |
1821052 | TORRES-ALBA     | 69         | PBC_NEW_238         | 2           | N   | 132.46762  | -17.43008   |
1821052 | TORRES-ALBA     | 70         | PBC_NEW_240         | 2           | N   | 53.18529   | 33.41111    |
1821052 | TORRES-ALBA     | 71         | PBC_NEW_246         | 2           | N   | 313.1335   | -28.14008   |
1821052 | TORRES-ALBA     | 72         | PBC_NEW_250         | 2           | N   | 308.298    | -17.89833   |
1821052 | TORRES-ALBA     | 73         | PBC_NEW_251         | 2           | N   | 285.80842  | -49.40369   |
1821052 | TORRES-ALBA     | 74         | PBC_NEW_257         | 2           | N   | 254.60721  | 68.85103    |
1821052 | TORRES-ALBA     | 75         | PBC_NEW_258         | 2           | N   | 314.3575   | -46.27664   |
1821052 | TORRES-ALBA     | 76         | PBC_NEW_263         | 2           | N   | 131.05458  | -14.12294   |
1821052 | TORRES-ALBA     | 77         | PBC_NEW_266         | 2           | N   | 34.11158   | 23.63058    |
1821052 | TORRES-ALBA     | 78         | PBC_NEW_267         | 2           | N   | 64.74312   | -74.52492   |
1821052 | TORRES-ALBA     | 79         | PBC_NEW_268         | 2           | N   | 25.18437   | 46.3935     |
1821052 | TORRES-ALBA     | 80         | PBC_NEW_269         | 2           | N   | 262.30883  | -53.52167   |
1821052 | TORRES-ALBA     | 81         | PBC_NEW_271         | 2           | N   | 183.56058  | 76.8025     |
1821052 | TORRES-ALBA     | 82         | PBC_NEW_272         | 2           | N   | 103.82046  | 53.15033    |
1821052 | TORRES-ALBA     | 83         | PBC_NEW_273         | 2           | N   | 339.44538  | -61.2645    |
1821052 | TORRES-ALBA     | 84         | PBC_NEW_277         | 2           | N   | 246.67096  | 82.86194    |
1821052 | TORRES-ALBA     | 85         | PBC_NEW_279         | 2           | N   | 304.88875  | 1.08086     |
1821052 | TORRES-ALBA     | 86         | PBC_NEW_280         | 2           | N   | 181.09908  | 17.03836    |
1821052 | TORRES-ALBA     | 87         | PBC_NEW_281         | 2           | N   | 237.10825  | -17.33428   |
1821052 | TORRES-ALBA     | 88         | PBC_NEW_286         | 2           | N   | 169.05196  | -42.56878   |
1821052 | TORRES-ALBA     | 89         | PBC_NEW_287         | 2           | N   | 348.44808  | 23.79175    |
1821052 | TORRES-ALBA     | 90         | PBC_NEW_291         | 2           | N   | 182.17779  | -30.8155    |
1821052 | TORRES-ALBA     | 91         | PBC_NEW_292         | 2           | N   | 206.92771  | -5.74633    |
1821052 | TORRES-ALBA     | 92         | PBC_NEW_293         | 2           | N   | 212.32971  | -38.79019   |
1821052 | TORRES-ALBA     | 93         | PBC_NEW_294         | 2           | N   | 187.13     | -15.52364   |
1821052 | TORRES-ALBA     | 94         | PBC_NEW_302         | 2           | N   | 246.71612  | -18.50072   |
1821052 | TORRES-ALBA     | 95         | PBC_NEW_303         | 2           | N   | 69.93521   | -34.51292   |
1821052 | TORRES-ALBA     | 96         | PBC_NEW_306         | 2           | N   | 156.57438  | 45.57236    |
1821052 | TORRES-ALBA     | 97         | PBC_NEW_307         | 2           | N   | 70.51592   | 61.98447    |
1821052 | TORRES-ALBA     | 98         | PBC_NEW_310         | 2           | N   | 113.54012  | 23.40539    |
1821052 | TORRES-ALBA     | 99         | PBC_NEW_318         | 2           | N   | 244.28642  | 23.04108    |
1821052 | TORRES-ALBA     | 100        | PBC_NEW_319         | 2           | N   | 47.46846   | -57.47994   |
1821052 | TORRES-ALBA     | 101        | PBC_NEW_320         | 2           | N   | 122.90721  | -11.77178   |
1821052 | TORRES-ALBA     | 102        | PBC_NEW_323         | 2           | N   | 218.12129  | 41.70142    |
1821052 | TORRES-ALBA     | 103        | PBC_NEW_326         | 2           | N   | 263.658    | 50.72717    |
1821052 | TORRES-ALBA     | 104        | PBC_NEW_330         | 2           | N   | 323.99871  | -16.28911   |
1821052 | TORRES-ALBA     | 105        | PBC_NEW_332         | 2           | N   | 344.85533  | 28.11631    |
1821052 | TORRES-ALBA     | 106        | PBC_NEW_336         | 2           | N   | 349.90087  | 11.64042    |
1821052 | TORRES-ALBA     | 107        | PBC_NEW_338         | 2           | N   | 29.05408   | 8.15853     |
1821052 | TORRES-ALBA     | 108        | PBC_NEW_339         | 2           | N   | 36.57567   | -74.46      |
1821052 | TORRES-ALBA     | 109        | PBC_NEW_341         | 2           | N   | 295.04521  | -55.17456   |
1821052 | TORRES-ALBA     | 110        | PBC_NEW_342         | 2           | N   | 113.2335   | 34.95528    |
1821052 | TORRES-ALBA     | 111        | PBC_NEW_343         | 2           | N   | 231.26783  | 49.34492    |
1821055 | DEGENAAR        | 1          | GALACTIC CENTER     | 490         | N   | 266.4      | -28.98333   |
1821061 | HOWARD          | 1          | WOLF 359            | 36          | N   | 164.1205   | 7.01472     |
1821061 | HOWARD          | 2          | ROSS 154            | 36          | N   | 282.45567  | -23.83625   |
1821061 | HOWARD          | 3          | ROSS 128            | 36          | N   | 176.935    | 0.80456     |
1821061 | HOWARD          | 4          | BARNARD'S STAR      | 36          | N   | 269.45208  | 4.69336     |
1821065 | MACCARONE       | 1          | SWIFT BULGE SURVEY  | 274         | N   | 266.41683  | -29.00783   |
1821074 | KAUR            | 1          | M87                 | 26          | N   | 187.70592  | 12.39111    |
1821075 | MARGUTTI        | 1          | FBOT1               | 90          | Y   | 0          | 0           |
1821087 | GELBORD         | 1          | MRK 817             | 365         | N   | 219.09196  | 58.79428    |
1821088 | HOMAN           | 1          | TRANSIENT 1         | 20          | Y   | 0          | 0           |
1821088 | HOMAN           | 2          | TRANSIENT 2         | 20          | Y   | 0          | 0           |
1821090 | VAN DEN EIJNDEN | 1          | TRANSIENT BEXRB     | 20          | Y   | 0          | 0           |
1821092 | OATES           | 1          | J221951-484240      | 144         | N   | 334.96583  | -48.71139   |
1821098 | SOKOLOVSKY      | 1          | NEW NOVA            | 40          | Y   | 0          | 0           |
1821101 | KRUMPE          | 1          | AGN IGNITION 1      | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 2          | AGN IGNITION 2      | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 3          | AGN IGNITION 3      | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 4          | AGN IGNITION 4      | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 5          | AGN IGNITION 5      | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 6          | AGN IGNITION 6      | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 7          | AGN IGNITION 7      | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 8          | AGN IGNITION 8      | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 9          | AGN IGNITION 9      | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 10         | AGN IGNITION 10     | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 11         | AGN IGNITION 11     | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 12         | AGN IGNITION 12     | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 13         | AGN IGNITION 13     | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 14         | AGN IGNITION 14     | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 15         | AGN IGNITION 15     | 2           | Y   | 0          | 0           |
1821101 | KRUMPE          | 16         | AGN SHUTDOWN 1      | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 17         | AGN SHUTDOWN 2      | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 18         | AGN SHUTDOWN 3      | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 19         | AGN SHUTDOWN 4      | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 20         | AGN SHUTDOWN 5      | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 21         | AGN SHUTDOWN 6      | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 22         | AGN SHUTDOWN 7      | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 23         | AGN SHUTDOWN 8      | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 24         | AGN SHUTDOWN 9      | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 25         | AGN SHUTDOWN 10     | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 26         | AGN SHUTDOWN 11     | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 27         | AGN SHUTDOWN 12     | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 28         | AGN SHUTDOWN 13     | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 29         | AGN SHUTDOWN 14     | 5           | Y   | 0          | 0           |
1821101 | KRUMPE          | 30         | AGN SHUTDOWN 15     | 5           | Y   | 0          | 0           |
1821102 | MILLER          | 1          | TYC 7091-888-1      | 1           | N   | 99.87638   | -32.40133   |
1821102 | MILLER          | 2          | V530 ORI            | 1           | N   | 91.14079   | -3.19781    |
1821102 | MILLER          | 3          | LL AQR              | 1           | N   | 338.67563  | -3.5995     |
1821102 | MILLER          | 4          | V501 HER            | 1           | N   | 263.93104  | 30.64308    |
1821102 | MILLER          | 5          | TYC 6511-1799-1     | 1           | N   | 97.35988   | -25.22483   |
1821102 | MILLER          | 6          | BK PEG              | 1           | N   | 356.78529  | 26.56667    |
1821102 | MILLER          | 7          | TYC 8590-374-1      | 1           | N   | 135.63183  | -56.88956   |
1821102 | MILLER          | 8          | BD+29 2091          | 1           | N   | 161.8465   | 28.39886    |
1821102 | MILLER          | 9          | HD074000            | 1           | N   | 130.21167  | -16.34514   |
1821102 | MILLER          | 10         | HD115169            | 1           | N   | 198.94746  | -29.50589   |
1821102 | MILLER          | 11         | HD200654            | 1           | N   | 316.64479  | -49.96397   |
1821102 | MILLER          | 12         | P041C               | 1           | N   | 222.99158  | 71.72147    |
1821102 | MILLER          | 13         | P177D               | 1           | N   | 239.80654  | 47.61164    |
1821102 | MILLER          | 14         | P330E               | 1           | N   | 247.89087  | 30.14622    |
1821102 | MILLER          | 15         | TYC 4424-1286-1     | 1           | N   | 263.21929  | 71.07864    |
1821102 | MILLER          | 16         | TYC 4212-455-1      | 1           | N   | 269.30513  | 67.06133    |
1821102 | MILLER          | 17         | TYC 4209-1396-1     | 1           | N   | 271.372    | 64.46447    |
1821102 | MILLER          | 18         | TYC 4433-1800-1     | 1           | N   | 272.14475  | 69.45797    |
1821102 | MILLER          | 19         | TYC 4205-1677-1     | 1           | N   | 273.03987  | 63.49508    |
1821108 | CORSI           | 1          | ZTFSN1              | 15          | Y   | 0          | 0           |
1821108 | CORSI           | 2          | ZTFSN1              | 15          | Y   | 0          | 0           |
1821108 | CORSI           | 3          | ZTFSN1              | 15          | Y   | 0          | 0           |
1821110 | CHELOUCHE       | 1          | MRK 279             | 360         | N   | 208.26438  | 69.30822    |
1821125 | WALTON          | 1          | NGC5907 ULX1        | 104         | N   | 228.99571  | 56.30303    |
1821134 | LAWTHER         | 1          | MRK 590             | 86          | Y   | 33.63992   | -0.76675    |
1821142 | SIEGEL          | 1          | M62                 | 50          | N   | 255.3025   | -30.11236   |
1821142 | SIEGEL          | 2          | M 15                | 25          | N   | 229.63842  | 2.08103     |
1821143 | JACKMAN         | 1          | CR DRA              | 150         | N   | 244.27225  | 55.26911    |
1821150 | SANTANDER       | 1          | NEUTRINO TARGET1    | 12          | Y   | 0          | 0           |
1821150 | SANTANDER       | 2          | NEUTRINO TARGET2    | 12          | Y   | 0          | 0           |
1821153 | PASHAM          | 1          | ERO-QPE1            | 75          | N   | 37.94692   | -10.33611   |
1821154 | SHAW            | 1          | UNKNOWN BH-LMXB     | 22          | Y   | 0          | 0           |
1821158 | JACKMAN         | 1          | L 168-9             | 30          | N   | 350.03133  | -60.06517   |
1821158 | JACKMAN         | 2          | TOI-776             | 30          | N   | 178.57663  | -37.55272   |
1821158 | JACKMAN         | 3          | TOI-1231            | 30          | N   | 156.74787  | -52.46942   |
1821158 | JACKMAN         | 4          | TOI-1201            | 30          | N   | 42.24696   | -14.53747   |
1821158 | JACKMAN         | 5          | TOI-1266            | 30          | N   | 197.99817  | 65.83381    |
1821161 | NICOTRA         | 1          | FRB1                | 16          | Y   | 0          | 0           |
1821161 | NICOTRA         | 2          | FRB2                | 16          | Y   | 0          | 0           |
1821162 | BROWN           | 1          | SN2018DFY-HOST      | 3           | N   | 325.88712  | 43.5495     |
1821162 | BROWN           | 2          | SN2018HFM-HOST      | 3           | N   | 144.03637  | 6.2575      |
1821162 | BROWN           | 3          | SN2018EVT-HOST      | 3           | N   | 206.66338  | -9.64333    |
1821162 | BROWN           | 4          | SN2018EVK-HOST      | 3           | N   | 348.93733  | 6.91103     |
1821162 | BROWN           | 5          | SN2018FEQ-HOST      | 3           | N   | 18.82804   | -44.91972   |
1821162 | BROWN           | 6          | SN2018FEB-HOST      | 3           | N   | 257.5465   | 21.64903    |
1821162 | BROWN           | 7          | SN2018BBL-HOST      | 3           | N   | 344.22679  | -37.34681   |
1821162 | BROWN           | 8          | SN2018GET-HOST      | 3           | N   | 113.53779  | 4.54942     |
1821162 | BROWN           | 9          | SN2018GRO-HOST      | 3           | N   | 332.955    | 38.70042    |
1821162 | BROWN           | 10         | SN2018GWO-HOST      | 3           | N   | 182.16213  | 68.77914    |
1821162 | BROWN           | 11         | SN2018HKX-HOST      | 3           | N   | 60.22421   | -66.67528   |
1821162 | BROWN           | 12         | SN2018HPU-HOST      | 3           | N   | 49.58842   | -41.60972   |
1821162 | BROWN           | 13         | SN2018ILU-HOST      | 3           | N   | 353.33742  | 4.80961     |
1821162 | BROWN           | 14         | SN2018BGV-HOST      | 3           | N   | 165.62621  | 55.59881    |
1821162 | BROWN           | 15         | SN2018HSO-HOST      | 3           | N   | 173.46637  | 53.11872    |
1821162 | BROWN           | 16         | SN2018HMX-HOST      | 3           | N   | 128.41392  | 55.59808    |
1821162 | BROWN           | 17         | SN2018HTR-HOST      | 3           | N   | 3.53317    | -23.16936   |
1821162 | BROWN           | 18         | SN2018HPU-HOST      | 3           | N   | 49.58842   | -41.60972   |
1821162 | BROWN           | 19         | SN2018HMX-HOST      | 3           | N   | 128.41392  | 55.59808    |
1821162 | BROWN           | 20         | SN2018JKY-HOST      | 3           | N   | 51.50879   | -17.56306   |
1821162 | BROWN           | 21         | SN2018JOV-HOST      | 3           | N   | 120.02975  | 58.70969    |
1821162 | BROWN           | 22         | SN2018HXF-HOST      | 3           | N   | 65.57483   | -5.46828    |
1821162 | BROWN           | 23         | SN2018IBB-HOST      | 3           | N   | 69.73733   | -20.66222   |
1821162 | BROWN           | 24         | SN2018IMF-HOST      | 3           | N   | 190.67246  | 13.26528    |
1821162 | BROWN           | 25         | SN2018ILU-HOST      | 3           | N   | 353.33742  | 4.80961     |
1821162 | BROWN           | 26         | SN2018ISQ-HOST      | 3           | N   | 49.21083   | 80.78458    |
1821162 | BROWN           | 27         | SN2018IVC-HOST      | 3           | N   | 40.67204   | -0.00889    |
1821162 | BROWN           | 28         | SN2018JAG-HOST      | 3           | N   | 15.95129   | 10.59236    |
1821162 | BROWN           | 29         | SN2018JKY-HOST      | 3           | N   | 51.50879   | -17.56306   |
1821162 | BROWN           | 30         | SN2018AAD-HOST      | 3           | N   | 59.50621   | -65.50694   |
1821162 | BROWN           | 31         | SN2018IVC-HOST      | 3           | N   | 40.67196   | -0.00886    |
1821162 | BROWN           | 32         | SN2018JOV-HOST      | 3           | N   | 120.02975  | 58.70969    |
1821162 | BROWN           | 33         | SN2018KPO-HOST      | 3           | N   | 55.17938   | -6.42333    |
1821162 | BROWN           | 34         | SN2018KZR-HOST      | 3           | N   | 127.22275  | 1.11075     |
1821162 | BROWN           | 35         | SN2018LEI-HOST      | 3           | N   | 38.39304   | -39.045     |
1821162 | BROWN           | 36         | SN2019BL-HOST       | 3           | N   | 106.14862  | 17.56961    |
1821162 | BROWN           | 37         | SN2019BM-HOST       | 3           | N   | 179.31808  | 36.41631    |
1821162 | BROWN           | 38         | SN2019KF-HOST       | 3           | N   | 156.82263  | 26.53308    |
1821162 | BROWN           | 39         | SN2019NP-HOST       | 3           | N   | 157.3415   | 29.51067    |
1821162 | BROWN           | 40         | SN2019RN-HOST       | 3           | N   | 34.49833   | 14.53344    |
1821162 | BROWN           | 41         | SN2019RZ-HOST       | 3           | N   | 102.60729  | 43.05331    |
1821162 | BROWN           | 42         | SN2019YZ-HOST       | 3           | N   | 235.48875  | 0.71094     |
1821162 | BROWN           | 43         | SN2019AHD-HOST      | 3           | N   | 162.79913  | 5.84203     |
1821162 | BROWN           | 44         | SN2019ARB-HOST      | 3           | N   | 184.88008  | 49.81414    |
1821162 | BROWN           | 45         | SN2019ATA-HOST      | 3           | N   | 153.54496  | -35.16083   |
1821162 | BROWN           | 46         | SN2019CAD-HOST      | 3           | N   | 137.17904  | 44.81278    |
1821162 | BROWN           | 47         | SN2019CCA-HOST      | 3           | N   | 180.71417  | -16.66333   |
1821162 | BROWN           | 48         | SN2019CQC-HOST      | 3           | N   | 275.42933  | 30.99261    |
1821162 | BROWN           | 49         | SN2019EIN-HOST      | 3           | N   | 208.37138  | 40.27539    |
1821162 | BROWN           | 50         | SN2019ENR-HOST      | 3           | N   | 143.69883  | 10.28689    |
1821162 | BROWN           | 51         | SN2019ENZ-HOST      | 3           | N   | 209.27537  | 27.99408    |
1821162 | BROWN           | 52         | SN2019ESA-HOST      | 3           | N   | 118.75367  | -76.41194   |
1821162 | BROWN           | 53         | SN2019HGE-HOST      | 3           | N   | 336.08833  | 24.78808    |
1821162 | BROWN           | 54         | SN2019EEZ-HOST      | 3           | N   | 94.09258   | -21.35994   |
1821162 | BROWN           | 55         | SN2019EHK-HOST      | 3           | N   | 185.73388  | 15.826      |
1821162 | BROWN           | 56         | SN2019EIN-HOST      | 3           | N   | 208.37138  | 40.27539    |
1821162 | BROWN           | 57         | SN2019ENR-HOST      | 3           | N   | 143.69883  | 10.28689    |
1821162 | BROWN           | 58         | SN2019FXY-HOST      | 3           | N   | 155.33737  | 12.17822    |
1821162 | BROWN           | 59         | SN2019GAF-HOST      | 3           | N   | 309.23017  | 2.80678     |
1821162 | BROWN           | 60         | SN2019GBX-HOST      | 3           | N   | 192.51167  | -14.76667   |
1821162 | BROWN           | 61         | SN2019HCC-HOST      | 3           | N   | 315.08721  | -21.34333   |
1821162 | BROWN           | 62         | SN2019JYW-HOST      | 3           | N   | 16.62592   | -2.19889    |
1821162 | BROWN           | 63         | SN2019KBJ-HOST      | 3           | N   | 332.84137  | 19.61764    |
1821162 | BROWN           | 64         | SN2019LSM-HOST      | 3           | N   | 218.76087  | 14.77711    |
1821162 | BROWN           | 65         | SN2019MUJ-HOST      | 3           | N   | 36.57717   | -9.83592    |
1821162 | BROWN           | 66         | SN2019NJV-HOST      | 3           | N   | 304.98829  | 15.37742    |
1821162 | BROWN           | 67         | SN2019NVM-HOST      | 3           | N   | 261.41108  | 59.44672    |
1821162 | BROWN           | 68         | SN2019NYK-HOST      | 3           | N   | 3.81333    | -8.18944    |
1821162 | BROWN           | 69         | SN2019ODF-HOST      | 3           | N   | 342.18617  | 27.57181    |
1821162 | BROWN           | 70         | SN2019ODP-HOST      | 3           | N   | 346.82954  | 13.85594    |
1821162 | BROWN           | 71         | SN2019OET-HOST      | 3           | N   | 343.98775  | -43.43858   |
1821162 | BROWN           | 72         | SN2019OFC-HOST      | 3           | N   | 23.40383   | -38.59972   |
1821162 | BROWN           | 73         | SN2019OVR-HOST      | 3           | N   | 112.20942  | 35.54756    |
1821162 | BROWN           | 74         | SN2019OYS-HOST      | 3           | N   | 106.99687  | 31.66536    |
1821162 | BROWN           | 75         | SN2019PJS-HOST      | 3           | N   | 271.16808  | 21.6345     |
1821162 | BROWN           | 76         | SN2019TUA-HOST      | 3           | N   | 329.50117  | 24.26586    |
1821162 | BROWN           | 77         | SN2019VXM-HOST      | 3           | N   | 299.61929  | 62.13778    |
1821162 | BROWN           | 78         | SN2019WBG-HOST      | 3           | N   | 180.678    | 1.98433     |
1821162 | BROWN           | 79         | SN2019WEP-HOST      | 3           | N   | 166.15412  | 45.97764    |
1821162 | BROWN           | 80         | SN2019XDF-HOST      | 3           | N   | 141.96583  | 68.41178    |
1821162 | BROWN           | 81         | SN2019XTW-HOST      | 3           | N   | 40.89      | -38.62528   |
1821162 | BROWN           | 82         | SN2019VRQ-HOST      | 3           | N   | 46.08925   | -16.02417   |
1821162 | BROWN           | 83         | SN2019YVQ-HOST      | 3           | N   | 186.84037  | 64.79992    |
1821162 | BROWN           | 84         | SN2020MR-HOST       | 3           | N   | 132.51587  | 70.2925     |
1821162 | BROWN           | 85         | SN2020VG-HOST       | 3           | N   | 177.22683  | -4.68167    |
1821162 | BROWN           | 86         | SN2020AKF-HOST      | 3           | N   | 142.16504  | 38.56306    |
1821162 | BROWN           | 87         | SN2020AQE-HOST      | 3           | N   | 175.87408  | -16.79806   |
1821162 | BROWN           | 88         | SN2020BIG-HOST      | 3           | N   | 75.31579   | -14.02444   |
1821162 | BROWN           | 89         | SN2020BIO-HOST      | 3           | N   | 208.907    | 40.4775     |
1821162 | BROWN           | 90         | SN2020BPI-HOST      | 3           | N   | 200.87092  | 62.44617    |
1821162 | BROWN           | 91         | SN2020BVC-HOST      | 3           | N   | 218.48758  | 40.24392    |
1821162 | BROWN           | 92         | SN2020CUI-HOST      | 3           | N   | 170.58187  | -7.57972    |
1821162 | BROWN           | 93         | SN2020CWD-HOST      | 3           | N   | 91.74608   | -49.00694   |
1821162 | BROWN           | 94         | SN2020DHJ-HOST      | 3           | N   | 223.37654  | 17.28914    |
1821162 | BROWN           | 95         | SN2020DUL-HOST      | 3           | N   | 224.30792  | 49.67439    |
1821162 | BROWN           | 96         | SN2020EES-HOST      | 3           | N   | 201.81329  | 32.03361    |
1821162 | BROWN           | 97         | SN2020EKK-HOST      | 3           | N   | 251.18817  | 22.51333    |
1821162 | BROWN           | 98         | SN2020FXA-HOST      | 3           | N   | 233.63763  | 37.53383    |
1821162 | BROWN           | 99         | SN2020JDO-HOST      | 3           | N   | 273.93183  | 58.21522    |
1821162 | BROWN           | 100        | SN2020HVF-HOST      | 3           | N   | 170.36021  | 3.01467     |
1821162 | BROWN           | 101        | SN2020HVP-HOST      | 3           | N   | 245.43913  | -2.28917    |
1821162 | BROWN           | 102        | SN2020JFO-HOST      | 3           | N   | 185.46029  | 4.48169     |
1821162 | BROWN           | 103        | SN2020KYG-HOST      | 3           | N   | 197.91496  | 22.91553    |
1821162 | BROWN           | 104        | SN2020KPX-HOST      | 3           | N   | 234.54225  | 4.78072     |
1821162 | BROWN           | 105        | SN2020KYX-HOST      | 3           | N   | 243.43971  | 22.92064    |
1821162 | BROWN           | 106        | SN2020LIL-HOST      | 3           | N   | 219.49863  | 9.38853     |
1821162 | BROWN           | 107        | SN2020LLX-HOST      | 3           | N   | 328.05838  | -55.5625    |
1821162 | BROWN           | 108        | SN2020MJM-HOST      | 3           | N   | 217.37221  | -0.02167    |
1821162 | BROWN           | 109        | SN2020MR-HOST       | 3           | N   | 132.51587  | 70.2925     |
1821162 | BROWN           | 110        | SN2020NLB-HOST      | 3           | N   | 186.35075  | 18.20347    |
1821162 | BROWN           | 111        | SN2020NVB-HOST      | 3           | N   | 187.24496  | 3.57278     |
1821162 | BROWN           | 112        | SN2020NXT-HOST      | 3           | N   | 339.40096  | 35.00211    |
1821162 | BROWN           | 113        | SN2020NTA-HOST      | 3           | N   | 241.84725  | 13.89261    |
1821162 | BROWN           | 114        | SN2020PJJ-HOST      | 3           | N   | 207.67213  | 30.48903    |
1821162 | BROWN           | 115        | SN2020PST-HOST      | 3           | N   | 18.30013   | 2.28383     |
1821162 | BROWN           | 116        | SN2020QIC-HOST      | 3           | N   | 3.77337    | 43.34322    |
1821162 | BROWN           | 117        | SN2020RGZ-HOST      | 3           | N   | 273.00437  | 51.72458    |
1821162 | BROWN           | 118        | SN2020RLJ-HOST      | 3           | N   | 345.29     | 23.48719    |
1821162 | BROWN           | 119        | SN2018DFG-HOST      | 3           | N   | 211.64458  | -5.45083    |
1821168 | PENIL           | 1          | PKS 0208-512        | 24          | N   | 32.6925    | -51.01719   |
1821168 | PENIL           | 2          | S5 0716+714         | 12          | N   | 110.47271  | 71.34344    |
1821168 | PENIL           | 3          | PG 1553+113         | 12          | N   | 238.92933  | 11.19011    |
1821171 | BODEWITS        | 1          | C/2017K2            | 61.1        | N   | 0          | 0           |
1821172 | FOLEY           | 1          | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 2          | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 3          | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 4          | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 5          | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 6          | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 7          | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 8          | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 9          | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 10         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 11         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 12         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 13         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 14         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 15         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 16         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 17         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 18         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 19         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 20         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 21         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 22         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 23         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 24         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 25         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 26         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 27         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 28         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 29         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 30         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 31         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 32         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 33         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 34         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 35         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 36         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 37         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 38         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 39         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 40         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 41         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 42         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 43         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 44         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 45         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 46         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 47         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821172 | FOLEY           | 48         | TRANSIENT           | 9           | Y   | 0          | 0           |
1821173 | HOMAN           | 1          | NS TRANSIENT        | 48          | Y   | 0          | 0           |
1821174 | LAHA            | 1          | TOO                 | 96          | Y   | 0          | 0           |
1821190 | MCHARDY         | 1          | MCG+08-11-11        | 41          | N   | 88.72338   | 46.43933    |
1821190 | MCHARDY         | 2          | NGC 4151            | 44          | N   | 182.63575  | 39.40572    |
1821190 | MCHARDY         | 3          | NGC 7469            | 41          | N   | 345.81508  | 8.874       |
1821190 | MCHARDY         | 4          | NGC 5548            | 44          | N   | 214.49804  | 25.13678    |
1821190 | MCHARDY         | 5          | M81                 | 182         | N   | 148.88821  | 69.06528    |
1821191 | PASHAM          | 1          | QPOUT               | 50          | Y   | 0          | 0           |
1821199 | FOLEY           | 1          | SN1                 | 10          | Y   | 0          | 0           |
1821199 | FOLEY           | 2          | SN2                 | 10          | Y   | 0          | 0           |
1821199 | FOLEY           | 3          | SN3                 | 10          | Y   | 0          | 0           |
1821199 | FOLEY           | 4          | SN4                 | 10          | Y   | 0          | 0           |
1821199 | FOLEY           | 5          | SN5                 | 10          | Y   | 0          | 0           |
1821199 | FOLEY           | 6          | SN6                 | 10          | Y   | 0          | 0           |
1821203 | LIN             | 1          | HLX-1_2MASXJ0111-45 | 52          | N   | 17.69583   | -46.02556   |
1821204 | DONG            | 1          | DLT_1               | 36          | Y   | 0          | 0           |
1821204 | DONG            | 2          | DLT_2               | 36          | Y   | 0          | 0           |
1821204 | DONG            | 3          | DLT_3               | 36          | Y   | 0          | 0           |
1821204 | DONG            | 4          | DLT_4               | 36          | Y   | 0          | 0           |
1821204 | DONG            | 5          | DLT_5               | 36          | Y   | 0          | 0           |

Proposal Abstracts

1821006 / JAMIE KENNEA / PENNSYLVANIA STATE UNIVERSITY

"RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS IN CYCLE 18"

We seek to identify high-energy counterparts to Fast Radio Bursts, for which the progenitor systems and emission mechanism remain unknown. We propose extremely rapid response follow-up observations with XRT and UVOT for exceptionally bright and low dispersion measure (nearby) events and to save the BAT event data when the FRB position is within the BAT FOV. This proposal takes advantage of new enhancements to Swift s fast-response capability, and will leverage an MOU with the CHIME team to trigger on FRBs within seconds of detection, providing the earliest and deepest constraints on non-radio emission from FRBs, as well as the greatest chance of finding a counterpart. This will significantly enhance the science return of Swift, and help solve the mystery of FRBs.

1821015 / JAMIE KENNEA / PENNSYLVANIA STATE UNIVERSITY

"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 next 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 O2 and O3 we also propose to greatly enhance the Swift GW follow-up program with new initiatives. 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 refactoring the Swift observing plans for the higher rates and smaller localizations O4 will yield.

1821023 / NICOLA MASETTI / INAF BOLOGNA

"SWIFT SNAPSHOT SURVEY OF SUSPECT SYMBIOTIC STARS IN THE GALAH ARCHIVE (S^6-GALAH)"

Within the about 880,000 stars so far observed by the GALactic Archaeology with HERMES (GALAH) high-resolution spectroscopic survey, 40 symbiotic star candidates of the accreting-only variety were found. These objects were chosen among stars of late spectral type not affected by coherent radial pulsations and showing an Halpha emission with a peak in excess of 0.5 above the adjacent continuum level. This project proposes to observe all of these sources via a follow-up snapshot survey performed with Swift in order to confirm their nature via the detection of ultraviolet/X-ray emission using UVOT and XRT. Once confirmed as accreting symbiotic stars, these objects will double the number of known systems of this type.

1821026 / SLAVKO BOGDANOV / COLUMBIA UNIVERSITY

"SWIFT MONITORING OF NEARBY X-RAY BINARY-RADIO MILLISECOND PULSAR TRANSITION OBJECTS"

The identification of three binary millisecond pulsars transforming between accreting and rotation-powered states has finally closed the evolutionary missing link between low-mass X-ray binaries and recycled pulsars. These discoveries imply that their parent population, redbacks, may also be recycled pulsars that sporadically revert to/from a low-luminosity accreting phase. We propose a continuation of the dedicated Swift X-ray and UV monitoring campaign of all such nearby binary radio millisecond pulsars aimed at catching them in the act of switching to/from an accreting state. This effort would greatly aid in constraining key aspects of the poorly understood transition process of pulsars between accretion and rotation power.

1821027 / ALAN MARSCHER / BOSTON UNIVERSITY

"COMBINED SWIFT AND IXPE OBSERVATIONS OF BLAZARS"

The investigators propose to observe with the Swift XRT and UVOT blazars whose X-ray linear polarization will be measured by IXPE. The Swift observations will specify which blazars are bright enough to be detecte during an IXPE visibility window, and will provide X-ray and UVOT continuum spectra during the IXPE observations. This is part of an overall program to determine the contemporaneous polarization (at mm, optical, and X-ray frequencies) and radio to gamma-ray spectral energy distribution of blazars. Such information will determine the mechanism and location (relative to lower frequencies) of the X-ray emission, neither of which has been determined thus far. It will also test models for particle acceleration that results in high-energy emission in the relativistic jets of blazars.

1821033 / KATIE AUCHETTL / UNIVERSITY OF CALIFORNIA, SANTA CRUZ

"PROBING THE EARLY UV AND X-RAY EVOLUTION OF TDES"

Modern optical surveys are poised to find a number of tidal disruption events (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.

1821035 / KATIE AUCHETTL / UNIVERSITY OF CALIFORNIA, SANTA CRUZ

"BRIGHT OPTICAL TDES AND THEIR FINAL STAGES OF EVOLUTION"

Black holes (BH) at the centres of quiescent galaxies reveal themselves through tidal disruption events (TDEs), a luminous, accretion-powered transient. These rare events provide us with unique insights into the physics associated with accretion and the BH itself. For most TDEs, observations focus on the initial detection and follow-up of the flare, but studies of the late-time emission have revealed many surprises, indicating that TDEs undergo significant changes in their accretion and emission mechanisms as they evolve. However, without detailed monitoring at late-times the uncertainties in the final stages of TDE evolution are quite large. Here we propose to take advantage of Swift's multi-wavelength capabilities to monitor the late time emission of some of the brightest & closest TDEs.

1821042 / YONG SHENG / CLEMSON UNIVERSITY

"PHOTOMETRIC REDSHIFTS FOR FERMI BLAZARS WITH SWIFT/UVOT"

The class of AGNs called blazars, are prominent members of Fermi detected sources. The study of blazar evolution with redshift is important as they also provide a powerful diagnostic tool to study the evolution of the Extragalactic Background Light (EBL). Using blazars as cosmological probes requires knowledge of their redshift. We propose to jointly use Swift-UVOT and SARA-CT/ORM, a 0.65m and 1m telescope in Chile and Spain respectively, to derive photometric redshifts for sources above z~1.3. This method makes use of 10 UV-nIR filters, which allows for reliable redshift measurements. This project will deliver measurements of the Spectral Energy Distributions for 20 3FGL blazars and establish photometric redshifts for those with z > 1.3.

1821052 / NURIA TORRES-ALBA / CLEMSON UNIVERSITY

"THE LEGACY OF SWIFT-BAT: THE HARD X-RAY SKY"

The Swift-BAT survey is the only hard X-ray survey of the whole sky, and will likely remain so for a long time. Past editions of the BAT catalog have resulted in numerous publications, and allowed us to discover elusive source populations (e.g. obscured AGN and high-z blazars), and perform unique measurements (e.g. high-energy cutoff of local AGN). However, 50 months of data (1/3 of available exposure) remain unpublished. With this proposal, we aim to assign a counterpart to every extragalactic source newly detected by BAT in the last 50 months of observations, in order to publish the most sensitive hard X-ray catalog of extragalactic sources (BAT 150-month). This will allow the community to access 700 new BAT sources (43% increase), at the fainter end of the BAT sensitivity range.

1821055 / NATHALIE DEGENAAR / UNIVERSITY OF AMSTERDAM

"A SWIFT LEGACY: THE MONITORING CAMPAIGN OF THE GALACTIC CENTER"

The center of our Galaxy has been monitored with the Swift/XRT almost every day since 2006. The high cadence provides excellent means to capture X-ray flares from Sgr A*, to study the accretion properties of 16 transient X-ray binaries, and to discover new X-ray transients. We propose to continue this Swift legacy program in cycles 18-19 and request daily 1-ks observations that amount to 490 ks of total exposure time. Our main objectives are to: 1) collect and study new flares from Sgr A*, 2) to detect any changes in the flaring rate or persistent emission of the supermassive black hole, and 3) to apply accretion models to very-faint X-ray binaries to determine their disk sizes. Many other topics can be addressed by this program, so it is highly valuable for a broad community.

1821061 / WARD HOWARD / UNIVERSITY OF COLORADO, BOULDER

"A SWIFT AND ALMA VIEW OF THE ORIGIN AND IMPACT OF M-DWARF FLARES"

Recently, a large millimeter flare was detected from Proxima Cen. Since little is known about millimeter flares, we have been given access to 40 hours of upcoming ALMA ACA Cycle 8 observations from private consultation to determine UV-millimeter flare relationships using 4 nearby M-dwarfs of various ages and activity levels. We propose to obtain simultaneous UV/X-ray coverage with Swift in order to better constrain the high-energy emission of millimeter flares and their potential impact on planetary habitability. Recent results suggest that UV and millimeter trace each other closely, and this proposed study will show if this is a universal property of mid-M dwarfs regardless of age, thereby creating a powerful new tool to determine the UV/X-ray environment of stars.

1821065 / THOMAS MACCARONE / TEXAS TECH UNIVERSITY

"THE SWIFT GALACTIC BULGE MONITORING SURVEY: FOURTH EPOCH"

We propose to survey a 16 square degree region of the Galactic Bulge, every two weeks during the part of the year when the survey region is observable to Swift. This will allow us to detect new very faint X-ray transients -- objects bright enough that they must be X-ray binaries, but too faint to be detected by all sky instruments. These objects are likely to dominate the total number of X-ray binaries, but they are still known in small numbers due to their faintness. We expect to substantially increase the number of know VFXTs, while also obtaining detections outside the hard-to-follow-up Galactic Center region where most of the currently known VFXTs have been found.

1821074 / AMANPREET KAUR / PENNSYLVANIA STATE UNIVERSITY

"EXPLORING UNPROBED X-RAY VARIABILITY IN M87 DURING THE 2022 EVENT HORIZON TELESCOPE (EHT) MULTIWAVELENGTH CAMPAIGN USING"

Understanding the accretion flows and the radiative output seen from the jets in active galactic nuclei are fundamental to our understanding of accreting black holes. As an AGN with a prominent jet visible in various energy regimes, M87 is a unique source to conduct these studies. The proposed investigation is to obtain Swift X-ray observations during the upcoming 2022 Event Horizon Telescope campaign collaborating with various facilities from radio to gamma-rays. Our goal is to capture the intrinsic variability in the X-ray emission throughout this campaign, which would be utilized to constrain the models explaining the observed spectral energy distribution for M87*. We request one observation (1ksec each) every day for 4 weeks during the entire length of the EHT campaign of 4 weeks.

1821075 / RAFFAELLA MARGUTTI / UNIVERSITY OF CALIFORNIA, BERKELEY

"A SWIFT INVESTIGATION OF FAST BLUE OPTICAL TRANSIENTS"

Fast and Blue Optical Transients (FBOTs) are a new class of stellar explosions. With extremely rapid time scales of evolution and luminous emission, FBOTs probe the extremes of the explosion parameters and/or stellar progenitor properties, and are hard to reconcile within the traditional supernova models. Alternative scenarios include strong shock interaction with a dense medium, or the presence of a central engine (e.g. BH or magnetar formed by the explosion). Here we propose a focused investigation of the closest FBOTs (d< 300 Mpc) with Swift as part of our 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.

1821087 / JONATHAN GELBORD / SPECTRAL SCIENCES, INC.

"EXTENDED MONITORING OF THE DRAMATICALLY-VARYING AGN MRK 817"

Mrk 817 is currently the subject of an ambitious 15-month, multi-observatory intensive reverberation mapping campaign, yielding constraints on the accretion disk and revealing new obscuration with dramatic variability. More time is needed to constrain the physical extent of the reprocessing region, apply new tests to separate the signals of the accretion disk and the broad line region, monitor the physical changes and the response they provoke, and explore the surprisingly weak correlation between X-rays and longer wavelengths. We propose a Swift Key Project to extend monitoring with 365 1-ks observations over two years. Supporting ground-based data (already approved) would extend year-round coverage to near-IR wavelengths. These data will provide a lasting Swift legacy for years to come.

1821088 / JEROEN HOMAN / EUREKA SCIENTIFIC

"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.

1821090 / JAKOB VAN DEN EIJNDEN / OXFORD UNIVERSITY

"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 9 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.

1821092 / SAMANTHA OATES / UNIVERSITY OF BIRMINGHAM

"LATE TIME UV OBSERVATIONS OF J221951-484240: AN UNUSUAL TDE OR AGN"

We propose UV observations of J221951-484240 to observe the late time behaviour of this source. This blue transient was found by UVOT during the follow-up of Gravitational Wave event S190930t; a neutron star-black hole merger. The nature of J221951-484240 is unknown. At a redshift of z=0.5205, the energetics (~1e52 erg) and duration of this source make it rare. It is unique from all previous TDEs, AGN and SNe, and is therefore either the most extreme example of one of these objects or a completely new type of transient. Observations in Swift cycle 18 will provide the late time UV behaviour of this transient which will be important in determining the progenitor. Only Swift/UVOT can provide long term UV monitoring of the colour and temporal behaviour of this extraordinary transient.

1821098 / KIRILL SOKOLOVSKY / MICHIGAN STATE UNIVERSITY

"IN SEARCH OF SHOCKS IN NOVAE"

The theory predicts that shocks that power GeV $gamma$-rays in novae should emit most of their energy as X-rays. However the predicted bright X-ray emission was never observed. Whether this lack points to something fundamental about the shock physics, or is simply an issue of small-number statistics, is unclear. We request Swift monitoring (40ks split across 10 epochs) and NuSTAR snapshot (40ks single epoch) of a newly discovered bright Galactic nova to expand the sample of gamma-ray novae with exquisite X-ray light curves. The resulting data will be interpreted alongside multi-wavelength observations to better understand shocks in novae, particularly characterize the luminosity, duration, temperature, location, and absorbing column associated with these shocks.

1821101 / MIRKO KRUMPE / LEIBNIZ INSTITUTE FOR ASTROPHYSICS POTSDAM

"SWIFT FOLLOW-UP OF RARE AGN IGNITION AND SHUT-DOWN EVENTS DETECTED WITH EROSITA"

We ask for 30 ToOs on changing-look AGN (CLAGN) while they are undergoing either an accretion ignition or a shut-down event. Such rare events are being identified by eROSITA's all-sky X-ray surveys, which are currently ongoing until 2023, and which comprise the first systematic X-ray detections of CLAGN near the beginning of their transition phase. Combined with optical data, we will use Swift XRT and UVOT to monitor the multiband emission components on time scales shorter than six months. Such monitoring will allow the first systematic analysis to constrain the rate and extent of these drastic flux changes, which are signatures of the AGN duty cycle, and yield crucial constraints on how the structural components of the accretion flow evolve as a function of accretion rate.

1821102 / NICOLA MILLER / KEELE UNIVERSITY

"ABSOLUTE ULTRAVIOLET PHOTOMETRY OF ECLIPSING BINARY STARS"

Accurate effective temperature (Teff) estimates for stars are essential to many areas of astrophysics, including studies of stellar structure and evolution, Galactic population studies and exoplanet research. The current Teff scale for FGK stars is uncertain by about 80K. It is possible to directly measure the Teff of FGK stars in eclipsing binaries to an accuracy of better than 40K for both components by combining photometric light curves, parallax from Gaia and flux measurements from NIR to FUV. We will obtain absolute UVOT flux measurements of 7 eclipsing binary stars, the majority of which have not been previously observed in the UV, along with 12 flux standard stars. These observations will allow us to significantly expand the sample of benchmark stars with accurate Teff measurements.

1821108 / ALESSANDRA CORSI / TEXAS TECH UNIVERSITY

"A SEARCH FOR BL-IC SNE WITH X-RAY AFTERGLOWS USING ZTF+SWIFT"

The rare class of massive-star explosions dubbed broad-lined (BL) Type Ic supernovae (SNe), estimated to constitute only ~5% of the Ib/c (stripped-envelope core-collapse) SN population, is of special interest due to its relation to gamma-ray bursts (GRBs). What makes some BL-Ic SNe produce GRBs remains a mystery. Two key questions are yet to be answered: (i) Why do only a fraction of BL-Ic SNe have relativistic ejecta powering radio/X-ray afterglows? (ii) Are low-luminosity GRBs beamed? Our proposal aims to answer these questions via follow-up observations of SNe discovered by the Zwicky Transient Facility (ZTF), using the Neil Gehrels Swift observatory and the Jansky VLA. This program capitalizes on the overlap between Cycle 18 of Swift and years 1.5-2.5 of the 3-yr-long Phase II of ZTF.

1821110 / DORON CHELOUCHE / UNIVERSITY OF HAIFA

"SHEDDING LIGHT ON LIGHT ECHOES: MAPPING THE CONTINUUM EMITTING REGIONS IN MRK 279 USING SWIFT AND HST"

There is growing evidence that our understanding of accretion onto supermassive black holes during the quasar phase is incomplete, and that accretion disks are larger than theoretically predicted. This has far reaching implications for accretion physics in the general astrophysical context. Reverberation mapping (RM) has been proven successful in studying quasar interiors, which cannot be resolved by conventional imaging techniques. Here we propose to use Swift's proven capabilities in the field to carry out a high-fidelity RM campaign in the X-ray, UV, and optical bands on a particular source (Mrk279) for which optical data suggested a very different origin for the time-delays than commonly assumed. The proposed Swift campaign will be augmented by simultaneous HST spectroscopy.

1821125 / DOMINIC WALTON / UNIVERSITY OF CAMBRIDGE

"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 most of the last few years in an off-state, it is now more frequently returning to its ULX state, and is also showing evidence for its 78d cycle when it does. This presents a unique opportunity to test the Lense-Thirring interpretation for the super-orbital periods seen in ULX pulsars with continued Swift monitoring.

1821134 / DANIEL LAWTHER / UNIVERSITY OF ARIZONA

"CAPTURING THE RE-IGNITION OF THE BROAD LINE REGION IN MRK 590"

The changing-look AGN Mrk 590 is currently in a repeat flaring state and may soon lose its broad emission lines again. We wish to seize this rare opportunity to document, the onset of AGN activity, since this can lead to significant insight on the long-standing problem of how AGNs are triggered and fueled. As part of a larger HST+VLT study, we ask for a Swift program of up to 86ks, with monitoring every 2 weeks, coupled with a ToO triggered if the faint state is reached. The aim is to measure UV broad-line fluxes, constrain the UV-X-ray continuum emission from the accretion disk, and establish the threshold ionizing luminosity required for broad-line production, a key diagnostic that is still unknown. This allows us to test theoretical model predictions for the broad-line region physics.

1821142 / MICHAEL SIEGEL / PENNSYLVANIA STATE UNIVERSITY

"A SWIFT/UVOT STUDY OF RR LYRAE IN M62 AND M5"

RR Lyrae stars have enormous pulsations in the near ultraviolet (NUV). UV photometry is uniquely sensitive to the properties of RR Lyrae stars -- particularly temperature and surface gravity -- and gives unique insight into the astrophysics of pulsating stars -- particularly the role of the hydrogen ionization front and the presence of shocks. We propose a survey of RR Lyrae stars in two relatively metal-rich clusters that host abundant populations of RR Lyrae, including numerous first overtone pulsators which are ripe for further exploration in the NUV. They are ideal targets for exploring the properties of first overtone pulsators, the effects of reddening on RR Lyrae, the astrophysics of pulsating stars and the connection between period, metallicity and NUV luminosity.

1821143 / JAMES JACKMAN / ARIZONA STATE UNIVERSITY

"UNDERSTANDING THE DISCONNECT BETWEEN NUV AND WHITE-LIGHT FLARE EMISSION FROM LOW-MASS STARS WITH CR DRA"

NUV flare emission from low-mass stars may influence rocky exoplanet atmospheric photochemistry and the abundance of biosignatures, yet flares may provide the needed flux for prebiotic chemistry to occur on their surfaces. Due to the scarcity of measured NUV flare rates, many studies rely on using poorly tested empirical models to extrapolate white-light flare rates measured with TESS to the NUV. We propose to simultaneously observe the highly active bright M binary CR Dra with the Swift UVOT grism, TESS and ground-based photometry and spectroscopy to study the NUV spectra of white-light flares. We will constrain flare NUV line emission and test the accuracy of modelling the NUV activity of low-mass stars from TESS data alone, providing a vital resource for future habitability studies.

1821150 / MARCOS SANTANDER / UNIVERSITY OF ALABAMA

"PINGING DOWN NEUTRINO-BLAZAR EMITTERS WITH SWIFT"

Given their extremely energetic emission, gamma-ray blazars have long been suggested as sources capable of accelerating cosmic rays, and that therefore may also produce neutrinos. The detection of an IceCube high-energy neutrino in temporal and spatial coincidence with a flaring blazar has strengthened the case for these sources to be responsible for at least part of the high-energy astrophysical neutrino flux observed by IceCube. As hadronic models most often predict high X-ray fluxes, the Neil Gehrels Swift Observatory is uniquely positioned to test this hypothesis by performing follow-up observations of promising neutrino source candidates. These observations are therefore crucial in understanding the multiwavelength properties of blazars as candidate hadronic sources.

1821153 / DHEERAJ PASHAM / MASSACHUSSETS INSTITUTE OF TECHNOLOGY

"TRACKING THE LONG-TERM EVOLUTION OF QUASI-PERIODIC ERUPTIONS FROM THE NUCLEUS OF A PASSIVE GALAXY USING XRT MONITORING"

Quasi-Periodic Eruptions (QPEs) are high-amplitude, repeating X-ray flashes from external galaxies. They are a promising new phenomenon which could provide novel insights into accretion instabilities and/or interactions of orbiting bodies with AGN accretion flows. We request for 2 sets of high-cadence XRT monitoring observations (15 visits/day for 5 days per set) of QPEs from eRO-QPE1 discovered by NICER. Our goals are to 1) track the evolution of QPE properties, i.e., mean time between eruptions, amplitude, and coherence over a time span of 3 years, and 2) validate the current evidence for a 2:3:4 period resonance seen in existing Swift and NICER data. Our science goals require high-cadence X-ray monitoring and currently Swift is ideally-suited to perform such observations.

1821154 / AARAN SHAW / UNIVERSITY OF NEVADA, RENO

"BLACK HOLE JET LAUNCHING PHYSICS: TRIGGERING JWST WITH SWIFT"

Despite ~50 years of compact object studies in the Galaxy, the physics of relativistic jet launching remains an active and open field of research. Luckily, with the impending launch of JWST, a new parameter space is opening up in the field of jet-physics, allowing for the study of the spectral break above which the jet becomes optically thin on sub-second time scales, providing a crucial link between light and plasma properties. We are proposing to use the rapid X-ray follow-up capabilities of Swift to monitor the outburst decay of a Galactic Low-mass X-ray binary, ensuring it is in a jet-dominated state in order to trigger an already in-place JWST program to study the jet break at high time resolution.

1821158 / JAMES JACKMAN / ARIZONA STATE UNIVERSITY

"DO OPTICALLY QUIET M STARS SHOUT IN THE NUV?"

Exoplanets around optically quiet low-mass stars have been highlighted as prominent targets for atmospheric characterisation, in part due to the apparent lack of NUV emission from flares that may aid the formation of hazes and the dissociation of biosignatures. However, optical observations are only sensitive to rarer high energy flares and not frequent lower energy flares that can be detected in the NUV. We propose to observe five optically quiet M star planet hosts with Swift UVOT, each of which has been earmarked for future atmospheric characterisation with JWST. We will study the NUV activity of each star and measure the average NUV flare rate of inactive M stars, to provide vital information about the UV environments of the future targets for atmospheric characterisation with JWST.

1821161 / MARIA NICOTRA / ISTITUTO NAZIONALE DI ASTROFISICA

"CLOSING IN ON THE PROGENITORS OF FAST RADIO BURSTS"

Despite rapid observational progress, the nature of fast radio bursts and their progenitors remains unknown. We propose a multi-wavelength follow-up campaign in order to detect their counterparts and narrow down the range of possible models, closing in on their elusive progenitors.

1821162 / PETER BROWN / TEXAS A&M UNIVERSITY

"NOT DONE YET: TEMPLATE OBSERVATIONS TO COMPLETE"

The Swift Ultra-Violet/Optical Telescope (UVOT) has revolutionized the understanding of supernova (SN) behavior in the ultraviolet (UV). Swift has observed over 800 SNe, including examples of all major classes and subtypes. This has enabled detailed studies of individual objects and to discover differences within SN subgroups. Much of the original SN photometry is contaminated by the underlying host galaxy light. We propose reobserving the host galaxies of 119 Swift supernovae to obtain SN-free measurements of the host galaxy flux at the SN position. This will improve the accuracy and usefulness of the SN photometry already obtained.

1821168 / PABLO PENIL / CLEMSON UNIVERSITY

"SWIFT CHARACTERIZATION OF PERIODIC-EMISSION BLAZARS"

Blazar emissions are characterized by high variability in their gamma-ray emission, property extended to other wavelengths, enclosing the entire electromagnetic spectrum. This variability also is observed in different timescales, ranging from years to minutes. Some blazars present predictable temporal behavior, having periodic patterns in their emissions. This proposal will observe 3 blazars with 5sigma periodicity in their gamma-ray emissions. The Swift observations will help to determine the correlation between the gamma-ray fluxes and the X-ray and ultra-violet fluxes in these periodicity blazars. Combining both periodicity-correlation studies allows us to constraint the modeling topologies to explain the variability in the MWL LCs in blazars.

1821171 / DENNIS BODEWITS / AUBURN UNIVERSITY

"WHY WAS COMET C/2017 K2 ACTIVE AT RECORD-SETTING DISTANCES AND WHAT HAPPENS WHEN IT REACHES THE INNER SOLAR SYSTEM?"

We propose to use Swift/UVOT to characterize the activity of comet C/2017 K2 (PanSTARRS) as it passes the H2O snowline for the first time. This comet was discovered to be already highly active as far as 25 au from the Sun, where only hypervolatiles like CO, N2, and O2 can sublimate. Using a combination of UVOT imaging and grism spectroscopy, we will follow the chemical composition, volatile and dust mass loss rates of this object. The proposed Swift observations will resolve whether this comet is a rare, CO-rich comet, or whether it belongs to the hyperactive comets that spew out icy grains. These findings address the chemical composition of comets, are directly relevant to the study of storage and release of volatiles in icy moons, and for the study of the distribution of volatiles.

1821172 / RYAN FOLEY / UNIVERSITY OF CALIFORNIA, SANTA CRUZ

"EXTREMELY YOUNG TRANSIENTS"

Observations of supernovae (SNe) and transients within hours of explosion provide unique data about the exploding star, its circumstellar (CS) environment, and companions. Swift opens a rare window to the system before and while the SN overruns its CS material and companion. X-ray and UV observations probe the interaction between a SN and nearby gas/companion stars. UV observations of a young SN within hours of explosion provide additional information about the size of the progenitor star, the density of its outer layers, and how the star exploded. This Key Project aims to observe all discovered young transients, regardless of survey, providing a legacy for Swift and the entire community by dramatically increasing the number of extremely young transients.

1821173 / JEREON HOMAN / EUREKA SCIENTIFIC

"INVESTIGATING SHALLOW HEATING IN NEUTRON STAR CRUSTS"

Studying how the accretion-heated crust of a neutron star cools after an outburst yields valuable information about its structure and the nuclear reactions occurring in the neutron-rich, high density environment. Past studies have identified an unexpected and poorly understood source of shallow heating in the outer crust. Investigating how this heat is generated in the outer crustal layers requires dense coverage of the outburst decay and the first ~50 days of crustal cooling. Swift is uniquely equipped to achieve this. We propose 48 ks of Swift ToO observations, spread over 16 pointings of 3 ks each, to monitor a transient neutron star X-ray binary as it transitions from outburst to quiescence.

1821174 / SIBASISH LAHA / UNIVERSITY OF MARYLAND, BALTIMORE COUNTY

"CAUGHT IN THE ACT: A SWIFT TOO CAMPAIGN ON CHANGING-LOOK AGN"

Large-scale time-domain surveys have lead to the identification of new types of extreme variability in active galaxies, called "changing look" active galactic nuclei (CL-AGNs, hereafter). These extreme variations are not only characterized by orders-of-magnitude changes in the optical, UV, and X-ray luminosity of the source, but also a rapid transition between spectral states. The primary goal of this program is to capture and densely monitor the earliest phases of a new (TOO) CL-AGN event, at optical, UV, and X-rays with Swift UVOT and XRT, in order to provide the critical information on how this phenomenon is triggered and how AGN central engine works.

1821190 / IAN MCHARDY / UNIVERSITY OF SOUTHAMPTON

"THE X-RAY/RADIO LINK IN RADIO-QUIET AGN"

The origin of radio emission in 'radio quiet' (RQ), ie non-blazar, AGN, is almost completely unknown. The key to unravelling the physical mechanism is, as in the better understood X-ray binary systems, to determine the link between the X-ray and radio variations. E.g, for radio emission from a jet we expect a positive correlation but for radio from a corona, an anti-correlation. Although there is rapidly growing interest in this field, there are few useful observations. Our own preliminary observations show a possible change from correlated variability at low accretion rates to anti-correlated at high rates. Here we ask to complete an ambitious study of 5 RQ AGN, across a range of accretion rates, to clearly determine the X-ray/radio links and put this field on a much firmer footing.

1821191 / DHEERAJ PASHAM / MASSACHUSSETS INSTITUTE OF TECHNOLOGY

"CAPTURING QUASI-PERIODIC OUTFLOWS FROM A FUTURE AGN OUTBURST USING XRT AND UVOT MONITORING"

Ultrafast outflows (UFOs) with an enigmatic quasi-periodic variability of 8.5 days have recently been identified from an AGN X-ray outburst. The physical origin of these quasi-periodic outflows (QP-Outs) is unclear but time-resolved X-ray spectral analysis suggests that they are driven by quasi-periodic changes in the apparent strength of absorption by the UFOs. Following the discovery of this new AGN phenomenon, we propose XRT+UVOT monitoring (500 s each for 150 d; 50 ks) of a carefully selected future AGN outburst. Our goals are to 1) expand on the pilot study and understand the frequency and duty cycle of such events, and 2) understand the accretion disk's role with simultaneous UV monitoring. The science objectives require X-ray and UV monitoring which can only be facilitated by Swift.

1821197 / AMY GOTTLIEB / UNIVERSITY OF MARYLAND, COLLEGE PARK

"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 (< 2 s) 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.

1821199 / RYAN FOLEY / UNIVERSITY OF CALIFORNIA, SANTA CRUZ

"PROBING THE PROGENITOR METALLICITY OF TYPE IA SUPERNOVAE WITH EARLY-TIME UV SPECTROSCOPY"

Ultraviolet (UV) observations of Type Ia supernovae (SNe Ia) are useful for understanding progenitor systems and explosion physics. Theory suggests that progenitor metallicy differences have little effect on optical SN data, but significantly change UV spectra. To address this problem, Swift has obtained UV spectra of ~40 SNe Ia at peak brightness, the largest such sample to date. Data from this sample confirm theoretical predictions and also find that SN Ia UV spectra a week before peak appear to be much stronger metallicity indicators. However, the current early-time sample is too small for statistical analyses. We propose to obtain UV spectra of 6 SN Ia > 1 week before peak to better investigate the metallicity effect and improve the cosmological precision of SNe Ia.

1821203 / DACHENG LIN / NORTHEASTERN UNIVERSITY

"TWO UNIQUE SOURCES IN A ROW: ESO 243-49 HLX-1 AND A NEWBORN HARD TIDAL DISRUPTION EVENT"

We request 52x1 ks weekly snapshots of two very special neighboring objects simultaneously in Swift GI Cycle 18: the strong intermediate mass black hole (IMBH) candidate ESO 243-49 HLX-1 and a newborn rare hard tidal disruption event (TDE). For HLX-1, these data will be crucial to further understand 1) how the outburst separation time (likely tracing the aperiodic orbital period) evolves and 2) what the ultimate fate of the system will be (e.g. donor ejection). For the new TDE, we want to 1) search for new giant fast X-ray flares as seen in the past for this event and 2) constrain its long-term UV and X-ray evolution.

1821204 / YIZE DONG / UNIVERSITY OF CALIFORNIA, DAVIS

"HIGH-CADENCE UV LIGHT CURVES OF EXTREMELY YOUNG SUPERNOVAE"

In the hours after explosion, supernovae (SNe) provide clues about their progenitors and explosion mechanisms. We are conducting a 12-hour cadence SN search of nearby galaxies, supported by rapid ground-based imaging, spectroscopy, and now, ultra-rapid Hubble Space Telescope (HST) UV spectroscopy. For several events, our program and rapid ground-based follow-up have revealed early light curve features that point to shock breakout or interactions with circumstellar material or a companion star. Here we request rapid, high-cadence (~6 hours) UV light curves of all young SNe found within ~24 hours of explosion. This set of up to five SNe, combined with early HST UV spectroscopy for one SN, will directly constrain their progenitor systems and explosion physics.

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