Swift Cycle 19 Results
The lists below contain the proposals recommended by the Cycle 19 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 19 proposals for observation: Please note that the ROSES 2022 Appendix D.5 "Swift Guest Investigator Cycle 19" 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 19 ToO proposals may be triggered until March 31, 2024."
- 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.
Jump to:
Recommended Proposals
Prop PI Title
1922005 DEMASI PRECISE X-RAY RECONNAISSANCE OF NEW, UNSTUDIED CANDIDATE-ISOLATED NEUTRON STARS
1922017 MARGUTTI A PANCHROMATIC STUDY OF SUPER-LUMINOUS SUPERNOVAE
1922023 EVANS FOLLOW UP OF NEW X-RAY TRANSIENTS DETECTED BY LSXPS
1922035 HO THE LANDSCAPE OF RELATIVISTIC STELLAR EXPLOSIONS
1922036 MASETTI SWIFT SNAPSHOT SURVEY OF SUSPECT SYMBIOTIC STARS IN THE GALAH ARCHIVE (S^6-GALAH)
1922039 LAHA SWIFT+FAST SIMULTANEOUS TOO OBSERVATIONS OF REPEATING FAST RADIO BURSTS.
1922040 KENNEA IDENTIFYING THE ELECTROMAGNETIC COUNTERPARTS TO COSMIC NEUTRINO SOURCES
1922041 KENNEA RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS IN CYCLE 19
1922051 RIVERA SANDOVAL INVESTIGATING THE ORIGIN OF FAST-EVOLVING LUMINOUS TRANSIENTS
1922064 IZZO THE JET-COCOON EMISSION IN RELATIVISTIC TYPE IC-BL SUPERNOVAE
1922065 DEGENAAR THE NATURE AND ACCRETION FLOW PROPERTIES OF SUB-LUMINOUS X-RAY BINARIES
1922066 CORSI A SEARCH FOR SNE IC-BL WITH X-RAY AFTERGLOWS USING ZTF+SWIFT
1922067 DAINOTTI GAMMA-RAY BURSTS AS REDSHIFT ESTIMATORS VIA MACHINE LEARNING TOOLS AND AN ASSOCIATED
WEB-APP ALERT
1922068 PAYNE INVESTIGATING THE LONG-TERM TRENDS OF ASASSN-14KO'S PERIODIC FLARES
1922069 TUBIN SEARCHING FOR CLOSE SUPERMASSIVE BLACK HOLE BINARIES WITH EROSITA, SWIFT, AND XMM-NEWTON
1922072 YANG FURTHER SWIFT MONITORING OF A CANDIDATE SUPERMASSIVE BLACK HOLE BINARY APPROACHING
FINAL MERGER
1922082 KRUMPE SWIFT FOLLOW-UP OF DRAMATIC ACCRETION CHANGES IN AGN
1922087 FUERST SWIFT MONITORING OF THE ULTRA-LUMINOUS X-RAY PULSAR NGC 7793 P13
1922089 WALTON TESTING THE LENSE-THIRRING MODEL FOR ULX VARIABILITY WITH NGC5907 ULX1
1922094 BODEWITS THE ACTIVITY AND EVOLUTION OF OORT CLOUD COMETS
1922099 HOMAN OBSERVING THE EARLY RISE OF X-RAY TRANSIENTS WITH SWIFT
1922105 ZHAO BUILDING WITH SWIFT/XRT A SAMPLE OF LUMINOUS, HIGH-REDSHIFT QUASARS TO CONSTRAIN THE
PROPERTIES OF AGN CORONAE
1922112 ABDULGHANI CONSTRAINING THE DISTANCES TO TRANSIENT BLACK HOLE X-RAY BINARIES WITH SWIFT
1922118 MORI INVESTIGATING THE ORIGIN OF X-RAY EMISSION FROM THE EXOTIC BE + STRIPPED B STAR BINARY HR 6819
1922122 ROWE DECONTAMINATING THE SWIFT UV-GRISM SAMPLE OF CORE-COLLAPSE SUPERNOVAE
1922125 KENNEA KEY PROJECT: THE DETECTION AND MONITORING OF ELECTROMAGNETIC COUNTERPARTS OF GRAVITATIONAL
WAVE SOURCES WITH SWIFT IN O4
1922132 GELBORD AGN INSIGHTS FROM VARIABILITY: X-RAY AND UV POWER SPECTRA OF NGC 4395
1922134 SORIA A CANDIDATE INTERMEDIATE-MASS BLACK HOLE IN THE HALO OF NGC 6099
1922135 BELLM SWIFTLY CONFIRMING NEW OPTICAL/IR-DISCOVERED X-RAY TRANSIENTS
1922136 DONG SWIFT/XRT/BAT FOLLOW UP OF AN UNIQUE GALACTIC TRANSIENT SOURCE
1922139 SHENG PHOTOMETRIC REDSHIFTS WITH SWIFT/UVOT
1922142 PASHAM TRACKING THE LONG-TERM EVOLUTION OF QUASI-PERIODIC ERUPTIONS FROM THE NUCLEUS OF A PASSIVE
GALAXY USING XRT MONITORING
1922144 STERN UPPER MASS GAP BLACK HOLE MERGERS IN AGN ACCRETION DISKS
1922147 MARSCHER X-RAY FLUX, SPECTRA, AND POLARIZATION OF BLAZARS
1922148 PASHAM CONTINUED SWIFT MONITORING OF REPEATING STELLAR TIDAL DISRUPTION EVENTS: TOWARDS A
LEGACY DATASET
1922150 HINKLE EARLY-TIME UVOT AND XRT FOLLOW-UP OF BRIGHT TDES
1922160 GOKUS GAMMA-RAY FLARES OF HIGH-REDSHIFT BLAZARS
1922168 SHAW BLACK HOLE JET LAUNCHING PHYSICS: TRIGGERING JWST WITH SWIFT
1922173 KENNEA SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS IN CYCLE 19
1922174 FOLEY REDUCING TYPE IA SUPERNOVA DISTANCE BIASES BY SEPARATING REDDENING AND INTRINSIC COLOR
1922176 SAND HIGH-CADENCE UV LIGHT CURVES OF EXTREMELY YOUNG SUPERNOVAE
1922179 SANTANDER CHARACTERIZING POTENTIAL NEUTRINO-EMITTING BLAZARS WITH SWIFT
1922183 MCDANIEL SWIFT CHARACTERIZATION OF THREE VERY HIGH ENERGY GALACTIC SOURCES WITH BRIGHT ROSAT COUNTERPARTS
1922187 LAWTHER SIZING UP THE ACCRETION DISK IN A FLARING CHANGING-LOOK AGN
1922196 SANTANDER DISENTANGLING THE FERMI ISOTROPIC GAMMA-RAY BACKGROUND
1922200 PASHAM SWIFT+NICER OBSERVATIONS TO IDENTIFY AND STUDY COSMOLOGICAL BLACK HOLES TURNING ON
RELATIVISTIC JETS
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] | 1922005 | DEMASI | 1 | 2RXSJ013424.5+193313 | 3.7 | N | 23.60225 | 19.55372 | 1922005 | DEMASI | 2 | 2RXSJ031146.7+052359 | 3.8 | N | 47.94471 | 5.39989 | 1922005 | DEMASI | 3 | 2RXSJ032019.0+043448 | 2.1 | N | 50.07937 | 4.58006 | 1922005 | DEMASI | 4 | 2RXSJ041155.7+001448 | 3.6 | N | 62.98217 | 0.24683 | 1922005 | DEMASI | 5 | 2RXSJ054014.4-045625 | 3.8 | N | 85.06021 | -4.94044 | 1922005 | DEMASI | 6 | 2RXSJ083932.9+263225 | 3.7 | N | 129.88742 | 26.54042 | 1922005 | DEMASI | 7 | 2RXSJ084051.1+272410 | 3.1 | N | 130.21308 | 27.403 | 1922005 | DEMASI | 8 | 2RXSJ092055.5+175526 | 2.5 | N | 140.23142 | 17.92397 | 1922005 | DEMASI | 9 | 2RXSJ100228.3+241829 | 4.4 | N | 150.61829 | 24.30817 | 1922005 | DEMASI | 10 | 2RXSJ101449.9+004101 | 3.2 | N | 153.70829 | 0.68364 | 1922005 | DEMASI | 11 | 2RXSJ102252.9+542601 | 4.8 | N | 155.72071 | 54.43383 | 1922005 | DEMASI | 12 | 2RXSJ105039.0+001203 | 3.7 | N | 162.66271 | 0.20103 | 1922005 | DEMASI | 13 | 2RXSJ105725.0+270436 | 1.8 | N | 164.35421 | 27.07667 | 1922005 | DEMASI | 14 | 2RXSJ105740.0+385418 | 3.2 | N | 164.417 | 38.90514 | 1922005 | DEMASI | 15 | 1RXSJ120258.8+191512 | 4 | N | 180.745 | 19.25333 | 1922005 | DEMASI | 16 | 2RXSJ120626.7+554907 | 3 | N | 181.61158 | 55.81878 | 1922005 | DEMASI | 17 | 1RXSJ124340.2+075808 | 3.9 | N | 190.9175 | 7.96889 | 1922005 | DEMASI | 18 | 2RXSJ125000.1+094956 | 3.4 | N | 192.50079 | 9.83244 | 1922005 | DEMASI | 19 | 1RXSJ133111.4+433108 | 6.4 | N | 202.7975 | 43.51903 | 1922005 | DEMASI | 20 | 2RXSJ133929.6+422456 | 2.2 | N | 204.87342 | 42.41558 | 1922005 | DEMASI | 21 | 2RXSJ134329.3+232445 | 2.5 | N | 205.87229 | 23.41264 | 1922005 | DEMASI | 22 | 2RXSJ141223.5+542748 | 4.1 | N | 213.09808 | 54.46356 | 1922005 | DEMASI | 23 | 2RXSJ142131.5+641036 | 4 | N | 215.38158 | 64.17675 | 1922005 | DEMASI | 24 | 2RXSJ143436.9+433847 | 1.2 | N | 218.65392 | 43.64639 | 1922005 | DEMASI | 25 | 2RXSJ150846.1+291949 | 2.8 | N | 227.19221 | 29.33033 | 1922005 | DEMASI | 26 | 2RXSJ155949.5+533926 | 3.7 | N | 239.95658 | 53.65742 | 1922005 | DEMASI | 27 | 2RXSJ170040.4+644537 | 7.6 | N | 255.16858 | 64.76031 | 1922005 | DEMASI | 28 | 1RXSJ173738.6+534739 | 14.4 | N | 264.41079 | 53.79431 | 1922005 | DEMASI | 29 | 2RXSJ230317.0+130239 | 3.7 | N | 345.82092 | 13.04444 | 1922005 | DEMASI | 30 | 2RXSJ234546.5+053230 | 3.7 | N | 356.44379 | 5.54192 | 1922005 | DEMASI | 31 | 1RXSJ001523.5+080250 | 5.4 | N | 3.84792 | 8.04736 | 1922005 | DEMASI | 32 | 2RXSJ011908.7+051029 | 3.2 | N | 19.78633 | 5.17486 | 1922005 | DEMASI | 33 | 2RXSJ023846.1-064119 | 2.4 | N | 39.69242 | -6.68867 | 1922005 | DEMASI | 34 | 2RXSJ051541.7+010528 | 1 | N | 78.92379 | 1.09125 | 1922005 | DEMASI | 35 | 2RXSJ091745.4+585427 | 3.9 | N | 139.43929 | 58.90764 | 1922005 | DEMASI | 36 | 2RXSJ112719.3+591201 | 3.3 | N | 171.83058 | 59.20031 | 1922005 | DEMASI | 37 | 2RXSJ112915.2+092529 | 4.8 | N | 172.31358 | 9.42489 | 1922005 | DEMASI | 38 | 2RXSJ122415.8+362136 | 3.6 | N | 186.06629 | 36.36011 | 1922005 | DEMASI | 39 | 2RXSJ124654.3+634625 | 3 | N | 191.72629 | 63.77386 | 1922005 | DEMASI | 40 | 2RXSJ140253.8+191139 | 2.8 | N | 210.72429 | 19.19439 | 1922005 | DEMASI | 41 | 2RXSJ143930.0+342146 | 2.9 | N | 219.87542 | 34.36297 | 1922005 | DEMASI | 42 | 2RXSJ145025.4+553256 | 3.4 | N | 222.60608 | 55.54917 | 1922005 | DEMASI | 43 | 2RXSJ152627.4+174905 | 2.3 | N | 231.6145 | 17.81825 | 1922017 | MARGUTTI | 1 | SLSN1 | 110 | Y | 0 | 0 | 1922017 | MARGUTTI | 2 | SLSN2 | 110 | Y | 0 | 0 | 1922023 | EVANS | 1 | CONF TRANS 1 | 7 | Y | 0 | 0 | 1922023 | EVANS | 2 | CONF TRANS 2 | 7 | Y | 0 | 0 | 1922023 | EVANS | 3 | CONF TRANS 3 | 7 | Y | 0 | 0 | 1922023 | EVANS | 4 | CONF TRANS 4 | 28 | Y | 0 | 0 | 1922023 | EVANS | 5 | CONF TRANS 5 | 28 | Y | 0 | 0 | 1922023 | EVANS | 6 | CONF TRANS 6 | 35.5 | Y | 0 | 0 | 1922023 | EVANS | 7 | NEEDS FOLLOWUP 1 | 2 | Y | 0 | 0 | 1922023 | EVANS | 8 | NEEDS FOLLOWUP 2 | 2 | Y | 0 | 0 | 1922023 | EVANS | 9 | NEEDS FOLLOWUP 3 | 2 | Y | 0 | 0 | 1922023 | EVANS | 10 | NEEDS FOLLOWUP 4 | 2 | Y | 0 | 0 | 1922023 | EVANS | 11 | NEEDS FOLLOWUP 5 | 2 | Y | 0 | 0 | 1922023 | EVANS | 12 | NEEDS FOLLOWUP 6 | 2 | Y | 0 | 0 | 1922023 | EVANS | 13 | NEEDS FOLLOWUP 7 | 2 | Y | 0 | 0 | 1922023 | EVANS | 14 | NEEDS FOLLOWUP 8 | 2 | Y | 0 | 0 | 1922023 | EVANS | 15 | NEEDS FOLLOWUP 9 | 2 | Y | 0 | 0 | 1922023 | EVANS | 16 | NEEDS FOLLOWUP 10 | 2 | Y | 0 | 0 | 1922023 | EVANS | 17 | NEEDS FOLLOWUP 11 | 2 | Y | 0 | 0 | 1922035 | HO | 1 | ORPHAN AFTERGLOW | 8 | Y | 0 | 0 | 1922035 | HO | 2 | ORPHAN AFTERGLOW | 8 | Y | 0 | 0 | 1922035 | HO | 3 | LFBOT | 10 | Y | 0 | 0 | 1922036 | MASETTI | 1 | A2-001 | 1 | N | 11.48092 | 1.51219 | 1922036 | MASETTI | 2 | A2-023 | 1 | N | 75.21429 | 16.12406 | 1922036 | MASETTI | 3 | A2-025 | 1 | N | 77.01483 | 16.62944 | 1922036 | MASETTI | 4 | A2-038 | 1 | N | 98.87004 | -21.40475 | 1922036 | MASETTI | 5 | A2-039 | 1 | N | 98.96892 | -20.24803 | 1922036 | MASETTI | 6 | A2-045 | 1 | N | 123.36108 | -4.57286 | 1922036 | MASETTI | 7 | A2-052 | 1 | N | 126.76204 | 10.60092 | 1922036 | MASETTI | 8 | A2-053 | 1 | N | 126.87562 | 13.44086 | 1922036 | MASETTI | 9 | A2-058 | 1 | N | 129.81583 | -13.27336 | 1922036 | MASETTI | 10 | A2-061 | 1 | N | 132.95933 | -2.54489 | 1922036 | MASETTI | 11 | A2-067 | 1 | N | 137.08671 | -22.57164 | 1922036 | MASETTI | 12 | A2-068 | 1 | N | 140.64213 | -25.70525 | 1922036 | MASETTI | 13 | A2-071 | 1 | N | 150.17337 | -21.59853 | 1922036 | MASETTI | 14 | A2-075 | 1 | N | 158.23129 | 12.85844 | 1922036 | MASETTI | 15 | A2-081 | 1 | N | 182.04225 | -9.13133 | 1922036 | MASETTI | 16 | A2-082 | 1 | N | 184.21075 | -6.52203 | 1922036 | MASETTI | 17 | A2-090 | 1 | N | 205.62083 | -10.90294 | 1922036 | MASETTI | 18 | A2-091 | 1 | N | 208.81654 | -5.56378 | 1922036 | MASETTI | 19 | A2-100 | 1 | N | 230.85483 | -17.13392 | 1922036 | MASETTI | 20 | A2-101 | 1 | N | 230.95263 | -20.34314 | 1922036 | MASETTI | 21 | A2-109 | 1 | N | 234.19562 | -16.97475 | 1922036 | MASETTI | 22 | A2-111 | 1 | N | 234.22579 | -17.55569 | 1922036 | MASETTI | 23 | A2-114 | 1 | N | 234.51317 | -14.53853 | 1922036 | MASETTI | 24 | A2-184 | 1 | N | 246.97587 | 6.24481 | 1922036 | MASETTI | 25 | A2-216 | 1 | N | 254.12821 | -2.66875 | 1922036 | MASETTI | 26 | A2-220 | 1 | N | 255.33442 | -15.01639 | 1922036 | MASETTI | 27 | A2-225 | 1 | N | 256.98579 | -22.22431 | 1922036 | MASETTI | 28 | A2-228 | 1 | N | 257.71667 | -21.26658 | 1922036 | MASETTI | 29 | A2-240 | 1 | N | 268.59792 | 8.31472 | 1922036 | MASETTI | 30 | A2-250 | 1 | N | 273.05887 | 5.57986 | 1922036 | MASETTI | 31 | A2-251 | 1 | N | 273.18996 | 6.01633 | 1922036 | MASETTI | 32 | A2-286 | 1 | N | 284.46179 | -21.122 | 1922036 | MASETTI | 33 | A2-296 | 1 | N | 286.04063 | -20.91942 | 1922036 | MASETTI | 34 | A2-330 | 1 | N | 290.92121 | -10.75189 | 1922036 | MASETTI | 35 | A2-331 | 1 | N | 291.26025 | -18.27078 | 1922036 | MASETTI | 36 | A2-342 | 1 | N | 295.86325 | 2.16703 | 1922036 | MASETTI | 37 | A2-346 | 1 | N | 298.678 | 6.43131 | 1922036 | MASETTI | 38 | A2-356 | 1 | N | 318.12375 | 5.66186 | 1922036 | MASETTI | 39 | A2-361 | 1 | N | 327.16671 | -21.28733 | 1922036 | MASETTI | 40 | A2-362 | 1 | N | 333.30483 | 7.54439 | 1922039 | LAHA | 1 | TOO FRB | 50 | Y | 0 | 0 | 1922039 | LAHA | 2 | TOO FRB | 50 | Y | 0 | 0 | 1922040 | KENNEA | 1 | ICECUBE TRIGGER #1 | 3.5 | Y | 0 | 0 | 1922040 | KENNEA | 2 | ICECUBE TRIGGER #2 | 9.5 | Y | 0 | 0 | 1922040 | KENNEA | 3 | ICECUBE TRIGGER #3 | 18.5 | Y | 0 | 0 | 1922040 | KENNEA | 4 | KM3NET TRIGGER #1 | 3.5 | Y | 0 | 0 | 1922040 | KENNEA | 5 | KM3NET TRIGGER #2 | 9.5 | Y | 0 | 0 | 1922041 | KENNEA | 1 | FRB #1 | 2 | Y | 0 | 0 | 1922041 | KENNEA | 2 | FRB #2 | 2 | Y | 0 | 0 | 1922041 | KENNEA | 3 | FRB #3 | 2 | Y | 0 | 0 | 1922041 | KENNEA | 4 | FRB #4 | 2 | Y | 0 | 0 | 1922041 | KENNEA | 5 | FRB #5 | 2 | Y | 0 | 0 | 1922041 | KENNEA | 6 | FRB #6 | 2 | Y | 0 | 0 | 1922041 | KENNEA | 7 | FRB #7 | 2 | Y | 0 | 0 | 1922041 | KENNEA | 8 | FRB #8 | 2 | Y | 0 | 0 | 1922041 | KENNEA | 9 | FRB #9 | 2 | Y | 0 | 0 | 1922041 | KENNEA | 10 | FRB #10 | 2 | Y | 0 | 0 | 1922051 | RIVERA SANDOVAL | 1 | FELT1 | 101 | Y | 0 | 0 | 1922064 | IZZO | 1 | SN2023XXX | 9 | Y | 0 | 0 | 1922064 | IZZO | 2 | SN2023YYY | 9 | Y | 0 | 0 | 1922064 | IZZO | 3 | SN2023ZZZ | 9 | Y | 0 | 0 | 1922064 | IZZO | 4 | SN2023WWW | 9 | Y | 0 | 0 | 1922064 | IZZO | 5 | SN2023YYY | 9 | Y | 0 | 0 | 1922064 | IZZO | 6 | SN2023JJJ | 9 | Y | 0 | 0 | 1922064 | IZZO | 7 | SN2024XXX | 9 | Y | 0 | 0 | 1922064 | IZZO | 8 | SN2024YYY | 9 | Y | 0 | 0 | 1922065 | DEGENAAR | 1 | VFXT-1 | 25 | Y | 0 | 0 | 1922065 | DEGENAAR | 2 | VFXT-2 | 25 | Y | 0 | 0 | 1922066 | CORSI | 1 | SN1 | 15 | Y | 0 | 0 | 1922066 | CORSI | 2 | SN2 | 15 | Y | 0 | 0 | 1922066 | CORSI | 3 | SN3 | 15 | Y | 0 | 0 | 1922068 | PAYNE | 1 | ASASSN-14KO | 97.5 | N | 81.32525 | -46.00592 | 1922069 | TUBIN | 1 | SMBHB CANDIDATE 1 | 25 | Y | 0 | 0 | 1922069 | TUBIN | 2 | SMBHB CANDIDATE 2 | 25 | Y | 0 | 0 | 1922072 | YANG | 1 | SDSSJ1430+2303 | 202 | N | 217.56688 | 23.06233 | 1922082 | KRUMPE | 1 | AGN IGNITION 1 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 2 | AGN IGNITION 2 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 3 | AGN IGNITION 3 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 4 | AGN IGNITION 4 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 5 | AGN IGNITION 5 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 6 | AGN IGNITION 6 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 7 | AGN IGNITION 7 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 8 | AGN IGNITION 8 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 9 | AGN IGNITION 9 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 10 | AGN IGNITION 10 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 11 | AGN IGNITION 11 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 12 | AGN IGNITION 12 | 3 | Y | 0 | 0 | 1922082 | KRUMPE | 13 | AGN SHUTDOWN 1 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 14 | AGN SHUTDOWN 2 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 15 | AGN SHUTDOWN 3 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 16 | AGN SHUTDOWN 4 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 17 | AGN SHUTDOWN 5 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 18 | AGN SHUTDOWN 6 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 19 | AGN SHUTDOWN 7 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 20 | AGN SHUTDOWN 8 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 21 | AGN SHUTDOWN 9 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 22 | AGN SHUTDOWN 10 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 23 | AGN SHUTDOWN 11 | 6 | Y | 0 | 0 | 1922082 | KRUMPE | 24 | AGN SHUTDOWN 12 | 6 | Y | 0 | 0 | 1922087 | FUERST | 1 | NGC 7793 P13 | 61.5 | N | 359.46254 | -32.62406 | 1922089 | WALTON | 1 | NGC5907 ULX1 | 104 | N | 228.99571 | 56.30303 | 1922094 | BODEWITS | 1 | C2017K2 | 39 | N | 0 | 0 | 1922094 | BODEWITS | 2 | C2022E3 | 49.4 | N | 0 | 0 | 1922099 | HOMAN | 1 | TRANSIENT 1 | 20 | Y | 0 | 0 | 1922099 | HOMAN | 2 | TRANSIENT 2 | 20 | Y | 0 | 0 | 1922105 | ZHAO | 1 | WISEAJ0259-0411 | 2 | N | 44.87142 | -4.19297 | 1922105 | ZHAO | 2 | WISEAJ0923+1518 | 2 | N | 140.89367 | 15.30094 | 1922105 | ZHAO | 3 | WISEAJ2230+0309 | 2 | N | 337.69121 | 3.15519 | 1922105 | ZHAO | 4 | WISEAJ0809+4500 | 2 | N | 122.33913 | 45.01342 | 1922105 | ZHAO | 5 | WISEAJ0340+0016 | 2 | N | 55.03946 | 0.27892 | 1922105 | ZHAO | 6 | WISEAJ0035+0411 | 2 | N | 8.995 | 4.18606 | 1922105 | ZHAO | 7 | WISEAJ0059+2654 | 2 | N | 14.71608 | 26.91208 | 1922105 | ZHAO | 8 | WISEAJ0826+1310 | 2 | N | 126.63546 | 13.17958 | 1922105 | ZHAO | 9 | WISEAJ1122+0758 | 2 | N | 170.54821 | 7.97425 | 1922118 | MORI | 1 | HR 6819 | 60 | N | 274.28138 | -56.02336 | 1922122 | ROWE | 1 | SN2006JC | 3 | N | 139.33658 | 41.90908 | 1922122 | ROWE | 2 | SN2008M | 3 | N | 95.422 | -59.72928 | 1922122 | ROWE | 3 | SN2012AW | 3 | N | 160.974 | 11.67164 | 1922122 | ROWE | 4 | SN2013EJ | 3 | N | 24.20067 | 15.75861 | 1922122 | ROWE | 5 | SN2016GKG | 3 | N | 23.56017 | -29.44006 | 1922122 | ROWE | 6 | SN2016GKG | 3 | N | 23.56017 | -29.44006 | 1922122 | ROWE | 7 | SN2017EAW | 3 | N | 308.68433 | 60.19328 | 1922122 | ROWE | 8 | SN2017EAW | 3 | N | 308.68433 | 60.19328 | 1922122 | ROWE | 9 | SN2017EGM | 3 | N | 154.77342 | 46.45392 | 1922122 | ROWE | 10 | SN2007PK | 3 | N | 22.94612 | 33.61503 | 1922122 | ROWE | 11 | SN2011DH | 3 | N | 202.52133 | 47.16967 | 1922122 | ROWE | 12 | SN2011DH | 3 | N | 202.52133 | 47.16967 | 1922122 | ROWE | 13 | SN2011DH | 3 | N | 202.52133 | 47.16967 | 1922122 | ROWE | 14 | SN2014G | 3 | N | 163.64221 | 54.29914 | 1922122 | ROWE | 15 | SN2010JL | 3 | N | 145.72221 | 9.49494 | 1922122 | ROWE | 16 | SN2011HT | 3 | N | 152.04412 | 51.84917 | 1922122 | ROWE | 17 | SN2011HT | 3 | N | 152.04412 | 51.84917 | 1922122 | ROWE | 18 | SN2009IP | 3 | N | 335.78442 | -28.94789 | 1922122 | ROWE | 19 | SN2009IP | 3 | N | 335.78442 | -28.94789 | 1922122 | ROWE | 20 | SN2009IP | 3 | N | 335.78442 | -28.94789 | 1922122 | ROWE | 21 | SN2009IP | 3 | N | 335.78442 | -28.94789 | 1922122 | ROWE | 22 | SN2015BF | 3 | N | 351.20429 | 15.28111 | 1922122 | ROWE | 23 | SN2015BF | 3 | N | 351.20429 | 15.28111 | 1922122 | ROWE | 24 | SN2005CS | 3 | N | 202.46992 | 47.17658 | 1922122 | ROWE | 25 | SN2006BP | 3 | N | 178.48225 | 52.35261 | 1922122 | ROWE | 26 | SN2006BP | 3 | N | 178.48225 | 52.35261 | 1922122 | ROWE | 27 | SN2006BP | 3 | N | 178.48225 | 52.35261 | 1922122 | ROWE | 28 | SN2013AB | 3 | N | 218.18537 | 9.88675 | 1922125 | KENNEA | 1 | GW EM CANDIDATE #1 | 70 | Y | 0 | 0 | 1922125 | KENNEA | 2 | GW EM CANDIDATE #2 | 70 | Y | 0 | 0 | 1922125 | KENNEA | 3 | GW EM CANDIDATE #3 | 70 | Y | 0 | 0 | 1922132 | GELBORD | 1 | NGC 4395 | 233.6 | N | 186.45358 | 33.54686 | 1922132 | GELBORD | 2 | NGC 4395 | 36 | N | 186.45358 | 33.54686 | 1922134 | SORIA | 1 | NGC6099 X-1 | 12 | N | 243.89296 | 19.45219 | 1922135 | BELLM | 1 | GALACTIC TRANSIENT 1 | 2 | Y | 0 | 0 | 1922135 | BELLM | 2 | GALACTIC TRANSIENT 2 | 2 | Y | 0 | 0 | 1922135 | BELLM | 3 | GALACTIC TRANSIENT 3 | 2 | Y | 0 | 0 | 1922135 | BELLM | 4 | GALACTIC TRANSIENT 4 | 2 | Y | 0 | 0 | 1922135 | BELLM | 5 | GALACTIC TRANSIENT 5 | 2 | Y | 0 | 0 | 1922135 | BELLM | 6 | GALACTIC TRANSIENT 6 | 2 | Y | 0 | 0 | 1922135 | BELLM | 7 | GALACTIC TRANSIENT 7 | 2 | Y | 0 | 0 | 1922135 | BELLM | 8 | GALACTIC TRANSIENT 8 | 2 | Y | 0 | 0 | 1922135 | BELLM | 9 | GALACTIC TRANSIENT 9 | 20 | Y | 0 | 0 | 1922135 | BELLM | 10 | GALACTIC TRANSIENT A | 20 | Y | 0 | 0 | 1922136 | DONG | 1 | J0631+25 | 36 | N | 97.7735 | 25.38731 | 1922139 | SHENG | 1 | 3FGL J0820.4+3640 | 2 | N | 125.08413 | 36.66792 | 1922139 | SHENG | 2 | 3FGL J0832.6+4914 | 2 | N | 128.09675 | 49.2225 | 1922139 | SHENG | 3 | 3FGL J0834.7+4403 | 2 | N | 128.7425 | 44.06058 | 1922139 | SHENG | 4 | 3FGL J0839.6+3538 | 2 | N | 129.93067 | 35.66706 | 1922139 | SHENG | 5 | 3FGL J0925.7+3129 | 2 | N | 141.43187 | 31.453 | 1922139 | SHENG | 6 | 3FGL J0930.2+8612 | 2 | N | 142.42942 | 86.20592 | 1922139 | SHENG | 7 | 3FGL J0934.1+3933 | 2 | N | 143.52779 | 39.44225 | 1922139 | SHENG | 8 | 3FGL J1117.3+2546 | 2 | N | 169.41829 | 25.81281 | 1922139 | SHENG | 9 | 3FGL J1129.0+3705 | 2 | N | 172.30962 | 37.05497 | 1922139 | SHENG | 10 | 3FGL J1143.0+6123 | 2 | N | 175.80042 | 61.36967 | 1922139 | SHENG | 11 | 3FGL J1150.5+4155 | 2 | N | 177.64479 | 41.91111 | 1922139 | SHENG | 12 | 3FGL J1203.2+3847 | 2 | N | 180.73792 | 38.86303 | 1922139 | SHENG | 13 | 3FGL J1212.6+5135 | 2 | N | 183.25367 | 51.49328 | 1922139 | SHENG | 14 | 3FGL J1222.7+8041 | 2 | N | 185.91871 | 80.66786 | 1922139 | SHENG | 15 | 3FGL J1323.9+1405 | 2 | N | 200.99371 | 14.10031 | 1922139 | SHENG | 16 | 3FGL J1354.5+3705 | 2 | N | 208.61121 | 37.11517 | 1922139 | SHENG | 17 | 3FGL J1500.6+4750 | 2 | N | 225.20275 | 47.85431 | 1922139 | SHENG | 18 | 3FGL J1649.4+5238 | 2 | N | 252.35412 | 52.5875 | 1922139 | SHENG | 19 | 3FGL J1702.6+3116 | 2 | N | 255.66167 | 31.26297 | 1922139 | SHENG | 20 | 3FGL J1705.5+7134 | 2 | N | 256.19575 | 71.63822 | 1922142 | PASHAM | 1 | 2MASS_02314715-10201 | 75 | N | 37.94692 | -10.33611 | 1922144 | STERN | 1 | BBHCANDIDATE | 240 | Y | 0 | 0 | 1922147 | MARSCHER | 1 | MRK421 | 21 | N | 166.11379 | 38.20883 | 1922147 | MARSCHER | 2 | MRK501 | 21 | N | 253.46758 | 39.76017 | 1922147 | MARSCHER | 3 | 1ES1959+650 | 21 | N | 299.99942 | 65.1485 | 1922147 | MARSCHER | 4 | 3C273 | 7 | N | 187.27792 | 2.05239 | 1922147 | MARSCHER | 5 | PG1553+113 | 7 | N | 238.92933 | 11.19011 | 1922147 | MARSCHER | 6 | 3C454.3 | 9 | N | 343.49062 | 16.14822 | 1922147 | MARSCHER | 7 | 3C279 | 9 | N | 194.04654 | -5.78931 | 1922147 | MARSCHER | 8 | 1ES0229+200 | 9 | N | 38.20258 | 20.28819 | 1922147 | MARSCHER | 9 | 3C454.3 | 1 | N | 343.49062 | 16.14822 | 1922147 | MARSCHER | 10 | BL LAC | 2 | N | 330.68038 | 42.27778 | 1922147 | MARSCHER | 11 | PKS2155-30 | 1 | N | 329.71696 | -30.22558 | 1922147 | MARSCHER | 12 | 1ZW 187 | 1 | N | 262.07758 | 50.21961 | 1922147 | MARSCHER | 13 | 3C279 | 1 | N | 194.04654 | -5.78931 | 1922147 | MARSCHER | 14 | 1ES0229+200 | 1 | N | 38.20258 | 20.28819 | 1922147 | MARSCHER | 15 | J0211+1051 | 1 | N | 32.80492 | 10.85967 | 1922147 | MARSCHER | 16 | 0716+714 | 2 | N | 110.47271 | 71.34339 | 1922147 | MARSCHER | 17 | 1ES0033+595 | 2 | N | 8.969 | 59.8345 | 1922148 | PASHAM | 1 | AT2018FYK | 20 | N | 342.56704 | -44.864 | 1922148 | PASHAM | 2 | ERASSTJ045650.3-203 | 40 | N | 74.20758 | -20.62989 | 1922150 | HINKLE | 1 | NEW TDE 1 | 45 | Y | 0 | 0 | 1922150 | HINKLE | 2 | NEW TDE 2 | 45 | Y | 0 | 0 | 1922160 | GOKUS | 1 | HIGH-Z BLAZAR | 63 | Y | 0 | 0 | 1922168 | SHAW | 1 | UNKNOWN BH-LMXB | 22 | Y | 0 | 0 | 1922168 | SHAW | 2 | GX 339-4 | 22 | Y | 255.70579 | -48.78975 | 1922173 | KENNEA | 1 | MAXI TRANSIENT #1 | 1 | Y | 0 | 0 | 1922173 | KENNEA | 2 | MAXI TRANSIENT #2 | 1 | Y | 0 | 0 | 1922173 | KENNEA | 3 | MAXI TRANSIENT #3 | 1 | Y | 0 | 0 | 1922173 | KENNEA | 4 | MAXI TRANSIENT #4 | 2 | Y | 0 | 0 | 1922173 | KENNEA | 5 | MAXI TRANSIENT #5 | 2 | Y | 0 | 0 | 1922173 | KENNEA | 6 | MAXI TRANSIENT #6 | 2 | Y | 0 | 0 | 1922173 | KENNEA | 7 | MAXI TRANSIENT #1 | 3.5 | Y | 0 | 0 | 1922174 | FOLEY | 1 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 2 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 3 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 4 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 5 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 6 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 7 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 8 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 9 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 10 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 11 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 12 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 13 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 14 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 15 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 16 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 17 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 18 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 19 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 20 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 21 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 22 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 23 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 24 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 25 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 26 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 27 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 28 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 29 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 30 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 31 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 32 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 33 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 34 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 35 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 36 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 37 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 38 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 39 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 40 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 41 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 42 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 43 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 44 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 45 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 46 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 47 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 48 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 49 | SN | 17 | Y | 0 | 0 | 1922174 | FOLEY | 50 | SN | 17 | Y | 0 | 0 | 1922176 | SAND | 1 | SN_1 | 36 | Y | 0 | 0 | 1922176 | SAND | 2 | SN_2 | 36 | Y | 0 | 0 | 1922176 | SAND | 3 | SN_3 | 36 | Y | 0 | 0 | 1922176 | SAND | 4 | SN_4 | 36 | Y | 0 | 0 | 1922176 | SAND | 5 | SN_5 | 36 | Y | 0 | 0 | 1922179 | SANTANDER | 1 | NEUTRINO TARGET1 | 12 | Y | 0 | 0 | 1922179 | SANTANDER | 2 | NEUTRINO TARGET2 | 12 | Y | 0 | 0 | 1922183 | MCDANIEL | 1 | 3FHLJ2229.4+5349 | 10 | N | 337.36283 | 53.81975 | 1922183 | MCDANIEL | 2 | 3FHLJ1528.4-6730 | 10 | N | 232.04513 | -67.51564 | 1922183 | MCDANIEL | 3 | 3FHLJ1619.8-6315 | 10 | N | 244.96067 | -63.25878 | 1922187 | LAWTHER | 1 | MRK 590 | 72 | Y | 33.63992 | -0.76675 | 1922196 | SANTANDER | 1 | FERMI_HEP_1 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 2 | FERMI_HEP_2 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 3 | FERMI_HEP_3 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 4 | FERMI_HEP_4 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 5 | FERMI_HEP_5 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 6 | FERMI_HEP_6 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 7 | FERMI_HEP_7 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 8 | FERMI_HEP_8 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 9 | FERMI_HEP_9 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 10 | FERMI_HEP_10 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 11 | FERMI_HEP_11 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 12 | FERMI_HEP_12 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 13 | FERMI_HEP_13 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 14 | FERMI_HEP_14 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 15 | FERMI_HEP_15 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 16 | FERMI_HEP_16 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 17 | FERMI_HEP_17 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 18 | FERMI_HEP_18 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 19 | FERMI_HEP_19 | 2 | Y | 0 | 0 | 1922196 | SANTANDER | 20 | FERMI_HEP_20 | 2 | Y | 0 | 0 | 1922200 | PASHAM | 1 | JETTEDTDE | 40 | Y | 0 | 0 |
Proposal Abstracts
1922005 / DEMASI / UNIVERSITY OF WASHINGTON
"PRECISE X-RAY RECONNAISSANCE OF NEW, UNSTUDIED CANDIDATE-ISOLATED NEUTRON STARS"
Only nine radio-quiet isolated neutron stars that emit strongly in X-rays (XINSs) are known. The value of these rare objects lies in their potential to provide insight into neutron star atmospheres and cooling rates and the EOS for neutron degenerate matter; yet the current sample is small and disparate. Using 1RXS and 2RXS with expanded companion multi-wavelength surveys, we have extended previous searches for blank-field X-ray source candidate-XINSs, recovering 2 known XINSs while identifying 46 new, unstudied candidate-fields devoid of multi-wavelength counterparts. Modest initial Swift reconnaissance of 43 targets is proposed in order to pinpoint these RASS X-ray sources and to assess whether their fields are more rigorously blank and thus whether further follow-up may be warranted.
1922017 / MARGUTTI / UNIVERSITY OF CALIFORNIA (BERKELEY)
"A PANCHROMATIC STUDY OF SUPER-LUMINOUS SUPERNOVAE"
With peak luminosities L peak~10^45 erg/s, the new class of Super-Luminous supernovae (SLSNe) outshines standard SN explosions by a factor of ~10-100 and represent the death of the most massive stars. The nature of their exceptional luminosities is still unclear and requires exotic explosion mechanisms and/or peculiar sources of energy. Here we propose rapid textit{Swift} follow up of 2 newly-discovered SLSNe to map the UV and X-ray emission during the early evolutionary stages as part of our multi-wavelength effort through programs on the VLA, ALMA, Chandra and optical/NIR facilities. The final aim is to: (i) Pin down SLSNe energy source; (ii) Map the diversity of SLSNe progenitor stars and pre-explosion evolution.
1922023 / EVANS / UNIVERSITY OF LEICESTER
"FOLLOW UP OF NEW X-RAY TRANSIENTS DETECTED BY LSXPS"
The Swift-XRT team have recently launched a unique new service, the 'Living Swift-XRT Point Source Catalogue', comprising a constantly-updated catalog and near real-time transient detector [1]. This service facilitates the exploration of a new region of phase space in time-domain astronomy, giving for the first time the opportunity to carry out rapid follow up of enigmatic events such as fast X-ray transients, and quasi-periodic eruptions from galactic nucleii. We propose to exploit this ability using Swift to follow up newly-detected transients across X-ray, UV and optical wavelengths, to classify the events, constrain their physics, and motivate follow up with other facilities and wavelengths.
1922035 / HO / CORNELL UNIVERSITY
"THE LANDSCAPE OF RELATIVISTIC STELLAR EXPLOSIONS"
Decades of long-duration GRB observations have yielded important insights on massive-star evolution and the physics of relativistic outflows. However, discovering relativistic stellar explosions exclusively via gamma-rays imposes a severe selection bias. Within the last few years, wide-field optical surveys have made the discovery of relativistic stellar explosions outside the gamma-ray band routine for the first time, resulting in the discovery of diverse phenomena that lack any associated detected GRB, such as "fast blue optical transients" and "orphan" afterglows. Rapid-turnaround X-ray observations with a focusing X-ray instrument, uniquely possible with Swift, are essential for understanding the origin of these phenomena and their physical connection to GRBs.
1922036 / MASETTI / ISTITUTO NAZIONALE DI ASTROFISICA (INAF)
"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, 80 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 40 of these sources via a follow-up snapshot survey performed with Swift in order to confirm their nature through the detection of ultraviolet/X-ray emission using UVOT and XRT. Once confirmed as accreting symbiotic stars, these objects will at least double the number of known systems of this type.
1922039 / LAHA / UNIVERSITY OF MARYLAND (BALTIMORE COUNTY)
"SWIFT+FAST SIMULTANEOUS TOO OBSERVATIONS OF REPEATING FAST RADIO BURSTS."
The fast radio bursts (FRBs) are milli-second duration radio transients, the origin of which is still unknown. Possible mechanisms that could generate these highly coherent radio emission from FRBs involve a) neutron star magnetospheres and/or b) relativistic shocks far from the central energy of the source. To understand the origin of the FRBs we will monitor the two crucial aspects during their bursting phases: (A) Polarization signatures in radio band with FAST, and (B) detect any possible X-ray counterpart corresponding to the FRBs with Swift. Once triggered, we propose to observe TWO repeating FRBs, each with a total exposure of 50 ks with Swift-XRT + FAST, during their bursting phases, to detect any X-ray emission contemporaneous with the radio bursts from the FRBs.
1922040 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
"IDENTIFYING THE ELECTROMAGNETIC COUNTERPARTS TO COSMIC NEUTRINO SOURCES"
Swift is a powerful facility for multi-messenger astronomy, having identified the first EM counter- parts to both high-energy neutrino and gravitational wave events. We propose to observe the 90% error regions of well-localised neutrinos with a high probability of cosmological origin detected by IceCube and, for the first time, KM3NeT. We request a total of 131 ks of approved ToO time.
1922041 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
"RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS IN CYCLE 19"
We seek to identify high-energy counterparts to Fast Radio Bursts, for which the progenitor systems and emission mechanism remain unknown. We propose extremely rapid response follow-up observations with XRT and UVOT for exceptionally bright and low dispersion measure (nearby) events and to save the BAT event data when the FRB position is within the BAT FOV. This proposal takes advantage of new enhancements to Swift's fast-response capability, trigger on CHIME and other detected FRBs within seconds of detection, providing the earliest and deepestconstraints on non-radio emission from FRBs, as well as the greatest chance of finding a counterpart. This will significantly enhance the science return of \swift, and help solve the mystery of FRBs.
1922051 / RIVERA SANDOVAL / UNIVERSITY OF TEXAS RIO GRANDE VALLEY
"INVESTIGATING THE ORIGIN OF FAST-EVOLVING LUMINOUS TRANSIENTS"
In 2018 the discovery of the optical transient AT2018cow was a big breakthrough in the astronomical community given its unprecedented characteristics. It was the first Fast-Evolving Luminous Transient (FELT) to be discovered in real time and extensively studied at all wavelengths, which has led to several interpretations about its origin. Using Swift XRT and UVOT observations, it was determined that AT2018cow was a bright X-ray and UV transient with rapid X-ray variability, with timescales of even a few hours, and a peculiar X-ray spectrum. These characteristics were observed for the first time on a FELT. We propose to investigate the origin of FELTs by exploiting the rapid response and multi band coverage of Swift joined with the great capabilities of NuSTAR and the VLA.
1922064 / IZZO / NIELS BOHR INSTITUTE
"THE JET-COCOON EMISSION IN RELATIVISTIC TYPE IC-BL SUPERNOVAE"
We propose to observe with both the UVOT and the XRT the emission of newly-discovered type Ic broad-lined supernovae (Ic-BL SNe) showing early pre-SN emission. Here, we aim at characterizing their physical properties, in particular the evolution of the cocoon component: the rapidly-rotating compact remnant can power a collimated jet that propagates within the progenitor s stellar layers, giving rise to a cocoon spreading laterally to the jet itself. The cocoon will emit as a thermal component in X-rays, rapidly cooling to UV-optical wavelengths. A monitoring program with Swift of newly-discovered Ic-BL SNe will allow us to study 1) the very early evolution of the cocoon; 2) quantify the role of the jet in powering the relativistic SN, and 3) determine the presence of an off-axis afterglow.
1922065 / DEGENAAR / UNIVERSITEIT VAN AMSTERDAM
"THE NATURE AND ACCRETION FLOW PROPERTIES OF SUB-LUMINOUS X-RAY BINARIES"
Very-faint X-ray transients exhibit accretion outbursts with a peak X-ray luminosity much lower than that of other black hole and neutron star X-ray binaries. These objects trace a poorly understood accretion regime and may represent a missing population of short-period binaries or neutron stars that act as magnetic propellers. We propose 50 ks of Swift ToO monitoring and 14h of VLA radio observations to study the outbursts of two very-faint X-ray transients. These data are complemented by optical monitoring with rapidly schedulable 1-2 m telescopes and nIR spectroscopy with 8-m class telescopes. We aim to study the properties of their accretion in/outflow, elucidate the nature of individual sources, and ultimately determine the fractions of different types of systems among the population.
1922066 / CORSI / TEXAS TECH UNIVERSITY
"A SEARCH FOR SNE IC-BL 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 about 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 SNe Ic-BL produce GRBs remains a mystery. Two key questions are yet to be answered: (i) Why do only a fraction of SNe Ic-BL 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 19 of Swift and the last year of ZTF Phase II.
1922067 / DAINOTTI / BAY AREA ENVIRONMENTAL RESEARCH INSTITUTE
"GAMMA-RAY BURSTS AS REDSHIFT ESTIMATORS VIA MACHINE LEARNING TOOLS AND AN ASSOCIATED WEB-APP ALERT"
Gamma-Ray Bursts (GRB) can cast light on key topics in astrophysics: the evolution of star formation rate, especially of the Population III stars, and the metal content of early galaxies. To tackle such topics large redshift samples are needed. However, only 26% of the total GRBs observed by Swift have measured redshifts which are difficult to infer due to the limited observational time at large facilities. To solve this issue, we will use Swift's archival GRB data to train machine learning algorithms that can estimate the redshift using photometric properties. We will create a public online interactive user-friendly webpage to infer the redshift of new GRBs as soon as their properties are observed. We will send automatic alerts for high-z GRBs candidates for world-wide optical follow-up.
1922068 / PAYNE / UNIVERSITY OF HAWAII (MANOA)
"INVESTIGATING THE LONG-TERM TRENDS OF ASASSN-14KO'S PERIODIC FLARES"
ASASSN-14ko is an unusual transient in the nucleus of ESO253-G003 that undergoes periodic UV/optical flares every ~114 days in which, surprisingly, the X-ray emission fades. We propose obtaining Swift UVOT and XRT observations of three upcoming flares predicted to peak in the optical on May 2.2, 2023, August 16.4, 2023, and November 30.2, 2023 UT. Previous Swift observations have started to reveal long-term changes in the peak luminosity of the flares and continuing to investigate the evolution of these multi-wavelength trends is a key piece of the puzzle to uncover the nature of this unique object.
1922069 / TUBIN / LEIBNIZ-INSTITUT FUR ASTROPHYSIK POTSDAM (AIP)
"SEARCHING FOR CLOSE SUPERMASSIVE BLACK HOLE BINARIES WITH EROSITA, SWIFT, AND XMM-NEWTON"
eROSITA has completed four deep all-sky surveys (eRASS1-4), monitoring almost half a million AGN every six months. It has the capability to identify exceptional AGN with periodic X-ray flux signals. These objects are potential supermassive black hole binaries (SMBHB). We request ToO monitoring campaigns for up to two periodic AGN eROSITA-selected candidates to have them in place when eROSITA resumes. Each ToO consists of five individual pointings, 5 ks each, spaced roughly one month apart. The campaigns are needed to track the flux modulation waveform on a monthly time scale, accurately resolve the period, and determine the details of follow-up observations to confirm the binary nature. The most convincing case will be the target of a pre-approved 100 ks XMM-Newton observation.
1922072 / YANG / PERIMETER INSTITUTE FOR THEORETICAL PHYSICS
"FURTHER SWIFT MONITORING OF A CANDIDATE SUPERMASSIVE BLACK HOLE BINARY APPROACHING FINAL MERGER"
Recently, Jiang et al. has reported an unprecedented Supermassive black hole binary (SMBHB) candidate in nearby Seyfert galaxy SDSSJ1430+2303 by its optical chirping flares, predicting a final merger time within three years. A ten-month high-cadence Swift monitoring since its discovery, as well as accompanying optical observations, have revealed a complex variability behaviour awaiting to be further understood. We hereby propose to conduct continuous Swift monitoring of the unique system in cycle 19, which covers the most probable period of merger time. The proposed observations are essential for characterizing X-ray/UV light curves and for triggering timely coordinated observations, which are key steps to confirm the SMBHB merger scenario and explore the associated physics.
1922082 / KRUMPE / LEIBNIZ-INSTITUT FUR ASTROPHYSIK POTSDAM (AIP)
"SWIFT FOLLOW-UP OF DRAMATIC ACCRETION CHANGES IN AGN"
We ask for 24 ToOs to observe changing-look AGN (CLAGN) as they are undergoing accretion transitions. These rare events were originally identified by eROSITA's all-sky X-ray surveys, with ongoing transitions confirmed by high cadence optical programs. Combined with these optical data, we will use Swift XRT and UVOT to monitor the evolution of the multi-wavelength emission components of these AGN. Only an extended multi-wavelength monitoring program will allow the first systematic analysis of how strong accretion changes impact the various components of the AGN. This program will also reveal the underlying mechanism(s) responsible for the structural and luminosity changes.
1922087 / FUERST / EUROPEAN SPACE ASTRONOMY CENTRE (ESAC)
"SWIFT MONITORING OF THE ULTRA-LUMINOUS X-RAY PULSAR NGC 7793 P13"
One of the most interesting ultra-luminous X-ray pulsars (ULXPs) is NGC 7793 P13, which stands out owing to its high duty cycle of pulsations, as well as being the only ULX pulsar where we know both the nature of the companion star and the full orbital ephemeris. Here we propose to continue the Swift monitoring program of P13, adding to the data taken in the last AOs and making full use of the combined power of the XRT and the UVOT. These observations will allow us to follow-up on the known X-ray and UV flux periods of the system and investigate the duty cycle of low- or off-states, one of which occurred between 2020 2021. They will also allow us to monitor other bright and transient X-ray sources in NGC 7793, like the black-hole candidate P9.
1922089 / WALTON / UNIVERSITY OF HERTFORDSHIRE
"TESTING THE LENSE-THIRRING MODEL FOR ULX VARIABILITY WITH NGC5907 ULX1"
Following a series of remarkable recent discoveries, it is now clear that some of the ultraluminous X-ray source (ULX) population are actually powered by highly super-Eddington neutron stars. NGC5907 ULX1 is the most extreme of these, exhibiting a remarkable peak luminosity of ~1e41 erg/s, as well as X-ray off-states (where the flux drops by a factor of ~100 or more) and a clear ~78d super-orbital X-ray period when active. Although the source has spent much 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.
1922094 / BODEWITS / AUBURN UNIVERSITY
"THE ACTIVITY AND EVOLUTION OF OORT CLOUD COMETS"
We propose to use Swift UVOT to characterize the activity of two Oort cloud comets: one new, and one more evolved. Swift followed these two exceptional comets as they approached the Sun. Cycle 19 offers the opportunity to observe both comets as they recede from the Sun, allowing us to investigate whether the erosion of the nuclei s top layers altered their activity and the relative abundance of molecules in the coma. We will use grism spectroscopy and photometric imaging to measure production rates of OH, dust, and minor species over the course of their apparitions. Swift s unique capabilities will allow us to determine the evolution of the comets activity which can then be compared to storage and release of volatiles in comets of other age classes.
1922099 / HOMAN / EUREKA SCIENTIFIC INC.
"OBSERVING THE EARLY RISE OF X-RAY TRANSIENTS WITH SWIFT"
Observing campaigns of black hole and neutron star X-ray transients have long relied on triggers from X-ray all-sky monitors or wide-field cameras. Due to the limited sensitivity of these instruments, the early rising phase of outbursts is typically missed. Here we propose a Swift monitoring program of known transient LMXBs that is triggered by detections of optical outburst activity with the Faulkes Telescopes/XB-NEWS. This allows us to catch transients as they emerge from quiescence in UV and X-rays. Our aim is to test the disk-instability model in LMXBs, follow the early X-ray spectral/variability evolution of an outburst, and search for signs of extended absorbing structures. We request monitoring campaigns for two transients, each with 10 (2 ks) observations at a 2-day cadence.
1922105 / ZHAO / HARVARD-SMITHSONIAN CENTER FOR ASTROPHYSICS
"BUILDING WITH SWIFT/XRT A SAMPLE OF LUMINOUS, HIGH-REDSHIFT QUASARS TO CONSTRAIN THE PROPERTIES OF AGN CORONAE"
The primary X-ray emission observed in AGN is believed to be produced from a tiny region surrounding the SMBH, namely the corona. A critical coronal compactness versus temperature threshold is predicted above which any increase in the source luminosity would then generate positron-electron pairs rather than continue heating the coronal plasma. Current observations show that all local AGNs populate the region below this critical line. However, these models have rarely been probed by sources in the high-luminosity regime where the tightest can be made on the coronal models. Here, we propose to confirm the flux of 9 high-luminosity quasars (z>1) to significantly extend the current sample size of the high-luminosity quasars that can be used to best constrain the physics of AGN coronae.
1922112 / ABDULGHANI / MONTANA STATE UNIVERSITY
"CONSTRAINING THE DISTANCES TO TRANSIENT BLACK HOLE X-RAY BINARIES WITH SWIFT"
Revealing the intrinsic properties of transient Black hole X-ray binaries (BHXBs) requires good distance measurements. Current methods used for measuring the distance to these sources struggle with a number of limitations that make it challenging to keep up with recent discovery rates. In an effort to solve this problem, we propose to use a method based on X-ray spectral modelling to reliably constrain the distance of 34 BHXBs that were observed by the Swift-XRT. The method will be also be improved and its accuracy tested, so that it can be applied to any newly discovered typical transient BHXB. Finally, to facilitate the usage of this method, it will also be implemented in the form of an online tool available to the community.
1922118 / MORI / COLUMBIA UNIVERSITY
"INVESTIGATING THE ORIGIN OF X-RAY EMISSION FROM THE EXOTIC BE + STRIPPED B STAR BINARY HR 6819"
The Be phenomenon - rapidly rotating B stars with circumstellar disks - is believed to originate from mass and angular momentum transfer in binary interactions. The binary scenario predicts a (largely undetected) population of Be + stripped B binaries after the primary loses its H-rich envelope. HR 6819 is one such an exotic binary with a 40.3 day orbital period. Recent AstroSAT and Swift-XRT observations revealed highly variable, soft X-ray emission, making HR 6819 the only confirmed Be+sB binary with X-ray detections. The proposed Swift/XRT observations aim to (1) rule out two unlikely X-ray emission mechanisms such as Gamma Cas and B stars and (2) measure the X-ray spectral modulation with the orbit for investigating the wind-wind and wind-disk interactions in the binary.
1922122 / ROWE / TEXAS A&M UNIVERSITY
"DECONTAMINATING THE SWIFT UV-GRISM SAMPLE OF CORE-COLLAPSE SUPERNOVAE"
We propose to revisit the fields of 17 previously observed core-collapse supernovae (CC SNe) to gather UVOT UV-grism template images. These observations require 81ks of observing time and will decontaminate 387ks of existing UV-grism observations that are otherwise unreliable. The proposed observations will allow us to remove this contamination using a background subtraction method and make the entire UV-grism sample of CC SNe available for analysis. We are using CC SNe to create spectrophotometric templates, investigate degeneracies between temperature/ionization, reddening, and metallicity, and compare against optical observations of high-redshift supernovae.
1922125 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
"KEY PROJECT: THE DETECTION AND MONITORING OF ELECTROMAGNETIC COUNTERPARTS OF GRAVITATIONAL WAVE SOURCES WITH SWIFT IN O4"
We seek to identify and observe EM counterparts to GW events during the 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.
1922132 / GELBORD / SPECTRAL SCIENCES INC.
"AGN INSIGHTS FROM VARIABILITY: X-RAY AND UV POWER SPECTRA OF NGC 4395"
We propose a monitoring campaign to characterize the variability of NGC 4395. This AGN is uniquely suited for variability studies because it has an exceptionally low black hole mass, so the relevant timescales of its accretion system are correspondingly smaller and can be more readily observed. We request 270ks for a Swift Key Project to monitor NGC 4395 over 292 days in Cycles 19 and 20. With these data, we will test models for X-ray reprocessing and accretion disk structure, principally by measuring and interpreting power spectra and interband lags in X-rays, UV and optical. Supporting ground-based observations are already in progress. This experiment can only be done with Swift and would provide a lasting legacy for years to come.
1922134 / SORIA / INAF
"A CANDIDATE INTERMEDIATE-MASS BLACK HOLE IN THE HALO OF NGC 6099"
An intriguing point-like X-ray source has recently been discovered in the halo of the elliptical galaxy NGC 6099. Based on its peak luminosity L_X ~ 5 x 10^{42} erg/s and its soft disk-blackbody spectrum (kT_{in} ~ 0.2 keV), we argue that it is a strong intermediate-mass black hole candidate. We propose to monitor it with four Swift/XRT observations during Cycle 19, to check its current activity level, constrain its duty cycle, and plan deeper multiband follow-up observations.
1922135 / BELLM / UNIVERSITY OF WASHINGTON
"SWIFTLY CONFIRMING NEW OPTICAL/IR-DISCOVERED X-RAY TRANSIENTS"
Low-mass X-ray Binaries (LMXBs) typically show transient outbursts due to instabilities in their accretion disks. The resulting X-ray brightening has historically enabled discovery of new LMXBs by all-sky monitors. However, this selection creates a bias against discovery of the potentially larger population of intrinsically faint X-ray transients. Large new optical and infrared (OIR) time-domain surveys now provide a novel and sensitive means of searching for such transient systems. Candidate outbursts will be identified through filtering near-real-time OIR alert photometry. Swift TOO observations in the X-ray and UV will confirm the presence of high-energy emission and help classify the outbursting system.
1922136 / DONG / UNIVERSITY OF BRITISH COLUMBIA
"SWIFT/XRT/BAT FOLLOW UP OF AN UNIQUE GALACTIC TRANSIENT SOURCE"
We propose the use of SWIFT/XRT and SWIFT/BAT to observe a newly discovered new long-period magnetar candidate, J0631+25. We have detected unique wide timescale emission using the Canadian Hydrogen Mapping Experiment/Pulsar/FRB instrument and it bears striking resemblance to two recently discovered long-period magnetars, both of which have no high energy counterparts. If we are able to detect high energy emission from J0631+25 this would strongly constrain emission models for this new class of object. Furthermore, if we were to find periodic emissions from the source, this could suggest the class of progenitor object. We do not request any funding.
1922139 / SHENG / CLEMSON UNIVERSITY
"PHOTOMETRIC REDSHIFTS 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-optical 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.
1922142 / PASHAM / MASSACHUSETTS 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.
1922144 / STERN / NASA/JPL
"UPPER MASS GAP BLACK HOLE MERGERS IN AGN ACCRETION DISKS"
The accretion disks of AGN are promising locations for the merger of compact objects detected by gravitational wave (GW) observatories. Embedded within a baryon-rich, high density environment, mergers within AGN are also expected to produce an electromagnetic counterpart. Theory predicts a UV-bright flare lasting several weeks, appearing approximately one month after the GW event, with the brightness of the flare scaling with the mass of the merger. We propose Swift monitoring of massive (>100 M(sun)), GW events detected in O4. The proposed data will inform the physics of GW mergers and accretion disks, and reliable electromagnetic counterparts to GW events provide an independent means of measuring cosmic expansion using the GW signal as a standard siren.
1922147 / MARSCHER / BOSTON UNIVERSITY
"X-RAY FLUX, SPECTRA, AND POLARIZATION 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 determine which blazars are bright enough to be detected by IXPE, monitor the optical/UV/X-ray flux and spectral variability during the IXPE observations, and provide X-ray and UVOT continuum spectra during the IXPE observations. This is part of an overall program to compare the X-ray, optical, and mm-wave polarization and gamma-ray to mm-wave spectral energy distributions of blazars. Such information will be used to determine the mechanism and location (relative to lower frequencies) of the X-ray emission. It will also test models for particle acceleration that results in high-energy emission in the relativistic jets of blazars.
1922148 / PASHAM / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"CONTINUED SWIFT MONITORING OF REPEATING STELLAR TIDAL DISRUPTION EVENTS: TOWARDS A LEGACY DATASET"
We are requesting for Swift (X-ray+UV) monitoring of two X-ray and UV bright, repeating stellar tidal disruption events (TDEs) AT2018fyk (once a month for ~10 months: 20 ks) and eRASStJ045650 (once a week for ~10 months: 40 ks). Swift campaign over the past 4 years (2018-2022) has captured a second outburst from these TDEs which has been interpreted as the signature of a repeating partial disruption. Our main goals are 1) to capture the full evolution of AT2018fyk's second dimming and additional outbursts from eRASStJ045650, and 2) acquire X-ray and UV data during these subsequent outbursts and compare them with previous outbursts. Our goals require long-term monitoring capability, high X-ray sensitivity, and UV coverage. This makes Swift the only facility capable of performing this study.
1922150 / HINKLE / UNIVERSITY OF HAWAII (MANOA)
"EARLY-TIME UVOT AND XRT FOLLOW-UP OF BRIGHT TDES"
We propose to obtain Swift UVOT and XRT ToO observations of two m <=18 mag tidal disruption events (TDEs) discovered prior to peak light in Cycle 19. We request 30 - 60 epochs of observation with 1.5 - 3ks per epoch divided between the two targets, for a total of 90ks. In recent years, the number of bright TDEs detected shortly after beginning to brighten has increased dramatically, allowing for early-time observations that have not been previously possible. Swift observations have provided critical early-time data about TDE X-ray and UV emission, driving new theoretical models of TDE physics. The proposed observations would increase the number of TDEs with very-early Swift UV data from one to three.
1922160 / GOKUS / WASHINGTON UNIVERSITY IN ST. LOUIS
"GAMMA-RAY FLARES OF HIGH-REDSHIFT BLAZARS"
We propose a ToO observation and follow-up monitoring campaign of a high-redshift (z>=3) blazar during a gamma-ray flare detected by Fermi. We request a total exposure time of 63 ks, split into 14 observations. So far, only 12 high-z blazars have been detected in the gamma-ray band. Because the high-energy component of their SED peaks in the MeV range, simultaneous X-ray and gamma-ray observations are needed to constrain the location of their high-energy emission peak and luminosity. We propose to obtain simultaneous X-ray and optical/UV data with Swift during enhanced gamma-ray activity of a high-z blazar. The data will be complemented by radio observations. The resulting MWL data set will increase our understanding of the of the stages of SMBH growth and evolution in the early Universe.
1922168 / SHAW / UNIVERSITY OF NEVADA-RENO
"BLACK HOLE JET LAUNCHING PHYSICS: TRIGGERING JWST WITH SWIFT"
Despite ~50 years of Galactic compact object studies, the physics of relativistic jet launching remains an active and open field of research. Luckily, with the recent launch of JWST, a new parameter space is opening up in the field of jet-physics; sub-second timescale studies of the spectral break above the frequency which the jet becomes optically thin can now provide 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 two Galactic Low-mass X-ray binaries, ensuring sources are in a jet-dominated state for triggering an already in-place JWST program to study the jet break at high time resolution.
1922173 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
"SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS IN CYCLE 19"
We propose to use Swift to localize Galactic X-ray transients discovered by MAXI, the operational phase of which has been extended until 2024. MAXI scans almost the entire X-ray sky every ̃92 minutes, with a source detection sensitivity of ̃60 mCrab in one orbit and ̃15 mCrab in one day, discovering X-ray transients with 0.1-0.5 degree accuracies in the 2-20 keV energy band. Swift provides rapid follow-up of MAXI triggers and localization up to 1.4 error radius, which is vital for identifying any optical/radio counterpart. XRT observations will also provide measurements of the low energy X-ray spectra. UVOT data will provide astrometric corrections and possibly optical counterparts. Swift is proven to be uniquely capable in this task.
1922174 / FOLEY / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)
"REDUCING TYPE IA SUPERNOVA DISTANCE BIASES BY SEPARATING REDDENING AND INTRINSIC COLOR"
Accurate distance measurements and unbiased cosmological constraints from Type Ia supernovae (SNe Ia) rely on proper correction for line-of-sight host galaxy dust reddening. The current standard for measuring SN distances confounds dust reddening and the intrinsic color-luminosity correlation into a single SN color law, introducing a bias that is currently SN cosmology s most challenging systematic uncertainty. A 130-orbit Cycle 30 and 31 HST program will obtain late-time UV and NIR imaging of 100 SNe Ia to break the degeneracy. We propose to observe the sample overlapping with Swift Cycle 19 (50 SNe) to obtain UV light curves covering peak. We will then transfer the knowledge from the HST program to all SNe with rest-frame UV data near peak.
1922176 / SAND / UNIVERSITY OF ARIZONA
"HIGH-CADENCE UV LIGHT CURVES OF EXTREMELY YOUNG SUPERNOVAE"
In the hours after explosion, supernovae provide clues about their progenitors and explosion mechanisms. We are conducting a 12-hour cadence SN search, coupled to real-time ingestion of other transient streams, to identify SNe in nearby galaxies as young as possible -- all supported by rapid ground-based imaging, spectroscopy, and in some circumstances HST UV spectroscopy. Rapid ground-based follow-up reveals early light curve and spectroscopic features (which vary on several hour time scales) that point to shock breakout or interactions with CSM or a companion star. Here we request high-cadence (6 hrs) UV light curves of all young SNe found within 24 hours of explosion (within 40 Mpc). This set of up to five SNe will directly constrain their progenitor systems and explosion physics.
1922179 / SANTANDER / UNIVERSITY OF ALABAMA
"CHARACTERIZING POTENTIAL NEUTRINO-EMITTING BLAZARS 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.
1922183 / MCDANIEL / CLEMSON UNIVERSITY
"SWIFT CHARACTERIZATION OF THREE VERY HIGH ENERGY GALACTIC SOURCES WITH BRIGHT ROSAT COUNTERPARTS"
Very High Energy (VHE, >10 GeV) gamma rays provide a direct view of some of the most extreme environments in our Galaxy and are an excellent probe of non-thermal astrophysical processes. Studies of the non-thermal Galactic source population are essential to understand where and how the bulk of the cosmic rays are accelerated in our Galaxy. A uniform survey conducted by Fermi of the Galactic plane at >10GeV has detected more than 300 sources. We propose to observe with Swift the 3 new sources that are associated with bright ROSAT objects and bear the largest probability of being Galactic. The study of these sources with Swift will unveil new sites of particle acceleration and will allow us understand the physics behind VHE emitters.
1922187 / LAWTHER / UNIVERSITY OF ARIZONA
"SIZING UP THE ACCRETION DISK IN A FLARING CHANGING-LOOK AGN"
Mrk 590 is a changing-look AGN that recently reignited. Existing Swift monitoring observations with a ~3-day cadence reveal an unprecedentedly strong X-ray to UV correlation, and an anomalous X-ray to UV delay inconsistent with a central driving continuum. For these archival data, we see hints of a second reprocessing region; however, the time sampling is too sparse to fully separate the putative compact and extended reprocessors. The strong X-ray variability and UV response makes Mrk 590 an excellent candidate for a dedicated disk reverberation mapping (RM) campaign. Here, we propose a ToO RM campaign during a major flaring event. Intensive monitoring with XRT and UVOT will allow us to isolate the response of the thermal accretion disk, if present, and the extended reprocessor.
1922196 / SANTANDER / UNIVERSITY OF ALABAMA
"DISENTANGLING THE FERMI ISOTROPIC GAMMA-RAY BACKGROUND"
The origin of the diffuse isotropic gamma-ray background measured by the Fermi gamma-ray satellite at energies between 100 MeV and 820 GeV remains largely uncertain. Population studies indicate that most of the emission originates in a large number of extragalactic objects such as active galactic nuclei, star-forming galaxies, or radio galaxies too faint to be resolved as individual sources. We here propose a ToO program aimed at pinpointing AGN counterparts to VHE Fermi-LAT photons and therefore help constrain the composition of the IGRB at energies above 250 GeV.
1922200 / PASHAM / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"SWIFT+NICER OBSERVATIONS TO IDENTIFY AND STUDY COSMOLOGICAL BLACK HOLES TURNING ON RELATIVISTIC JETS"
Following Swift (XRT+UVOT) and NICER's recent success in capturing the spectro-timing variability of the farthest stellar tidal disruption event (TDE) to-date we propose ToO monitoring observations of a future relativistic TDE, i.e., a system with a newborn relativistic jet pointed directly along our line of sight. Our main goals are 1) to establish the relativistic nature of the future transient by measuring its luminosity and variability, and 2) combine NICER and Swift/UVOT data with our approved multi-frequency radio data to perform multi-epoch spectral energy distribution modelings to shed light on the underlying jet physics. Our scientific goals require high-cadence monitoring and optical/UV coverage for months making NICER+Swift ideal for the proposed study.
- Curator: J.D. Myers
- NASA Official & Swift PI: Brad Cenko
- PAO Contact: Francis Reddy
- Questions/Comments/Feedback
- › Privacy Policy and Important Notices
- › Accessibility
- › Contact NASA
- › Page Last Updated: Fri, Feb 10, 2023