The Neil Gehrels Swift Observatory

Swift Cycle 15 Results

The lists below contain the proposals recommended by the Cycle 15 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 15 proposals for observation: Please note that the ROSES 2018 Appendix D.5 "Swift Guest Investigator Cycle 15" 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/submit.html. If you have trouble submitting this form please email swiftods@swift.psu.edu.

"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 15 ToO proposals may be triggered until March 31, 2020."

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Recommended Proposals

Prop    PI              	Title

Key Projects: 
1518037 KARA                    SIMULTANEOUS DISC AND CORONA REVERBERATION MAPPING IN AGN MRK 335
1518159 MACCARONE               THE SWIFT GALACTIC BULGE MONITORING SURVEY: SECOND EPOCH
1518162 GELBORD                 INTENSIVE AGN DISK REVERBERATION MAPPING OF MRK 876 WITH SWIFT AND TESS
1518168 HOWELL                  MAXIMIZING SWIFT S IMPACT WITH THE GLOBAL SUPERNOVA PROJECT

Regular proposals: 
1518002 GRUPE                   CATCHING AGN IN EXTREME X-RAY FLUX STATES
1518022 KENNEA                  SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS
1518027 VAN DEN EIJNDEN         THE NATURE AND ACCRETION FLOW PROPERTIES OF SUB-LUMINOUS X-RAY BINARIES
1518033 BOGDANOV                OBSERVING THE NEXT X-RAY BINARY-RADIO MILLISECOND PULSAR TRANSITION
1518057 FUERST                  SWIFT MONITORING OF NEUTRON STAR POWERED ULTRA-LUMINOUS X-RAY SOURCES
1518059 WARGELIN                PROXIMA CENTAURI'S STELLAR CYCLE
1518068 DEGENAAR                SWIFT/VLA MONITORING OF THE DECAY OF A GIANT BE/X-RAY BINARY OUTBURST
1518078 SAND                    HIGH CADENCE UV LIGHT CURVES OF EXTREMELY YOUNG SUPERNOVAE
1518089 SMITH                   THE MISSING PIECE OF THE PUZZLE: SWIFT MONITORING OF TESS-FERMI BLAZARS
1518099 URSINI                  TOWARDS A CENSUS OF THE ENERGETICS AND DUTY CYCLE OF GIANT RADIO GALAXIES
1518100 AUCHETTL                LATE TIME MONITORING OF BRIGHT AND NEARBY OPTICAL TDES
1518118 SAKAMOTO                SWIFT RAPID FOLLOW-UP OBSERVATIONS OF MAXI XRFS AND LLGRBS
1518131 TOHUVAVOHU              RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS
1518145 SANTANDER               PINPOINTING THE SOURCES OF THE FERMI ISOTROPIC GAMMA-RAY BACKGROUND
1518164 PALIYA                  THE QUEST FOR THE MOST EFFICIENT PARTICLE ACCELERATORS
1518170 PASHAM                  HIGH-CADENCE XRT MONITORING OF ULTRALUMINOUS X-RAY SOURCES TO SEARCH FOR ORBITAL PERIODS
1518177 MACGREGOR               THE ORIGIN AND IMPACT OF FLARES IN THE PROXIMA CENTAURI PLANETARY SYSTEM
1518180 HAGEN                   ENHANCING THE UVOT LEGACY: ENABLING EXTENDED SOURCE PHOTOMETRY
1518185 KEIVANI                 SEARCHING FOR X-RAY AND UV/O COUNTERPARTS OF GRAVITATIONAL WAVE AND HIGH-ENERGY NEUTRINO COINCIDENT
SIGNALS WITH SWIFT 1518186 TERRERAN EXPLOSION MECHANISMS AND ENERGY SOURCES POWERING SUPER-LUMINOUS SUPERNOVAE 1518191 AYALA SOLARES SWIFT FOLLOW-UP SEARCHES OF LOW FALSE ALARM RATE HIGH-ENERGY NEUTRINO + GAMMA-RAY COINCIDENCES 1518194 KUIN SWIFT ULTRAVIOLET SPECTROSCOPY OF TDE 1518199 HOMAN A RARE LOOK AT A BLACK HOLE TRANSIENT EMERGING FROM QUIESCENCE 1518200 FOLEY YOUNG SUPERNOVA EXPERIMENT 1518203 HENZE PROBING THE ERUPTION STATISTICS AND EVOLUTION OF THE UNIQUE RECURRENT NOVA M31N 2008-12A 1518206 D'ORAZIO FIRST X-RAY OBSERVATIONS OF A PECULIAR FLARING AGN OBSERVED BY KEPLER:
A SUPERMASSIVE BLACK HOLE BINARY HYPOTHESIS 1518215 MILNE UVOT CALIBRATION OF TYPE IA SUPERNOVA FIELDS: SEARCHING FOR GROUND-BASED EVIDENCE OF BI-MODALITY Fill-Ins: 1518214 BROWN NOT DONE YET: TEMPLATE OBSERVATIONS TO COMPLETE SWIFT SUPERNOVAE

Recommended Targets

Definition of Columns

  1. Proposal: Proposal number assigned by Swift mission
  2. PI: Principal Investigator's last name
  3. Target_Num: Target number as listed on the proposal form
  4. Target_Name: Target name as listed on proposal forms
  5. Time: Total observing time approved, in ksec
  6. ToO: "Y" if Target of Opportunity proposal, otherwise "N"
  7. RA: Right Ascension (equinox J2000) in degrees
  8. Dec: Declination (equinox J2000) in degrees


Prop   |PI              |Target_Num|Target_Name         |Time [ ks ]|TOO|RA [ deg ]|Dec [ deg ]|

1518037|KARA            |  1       |MRK 335             |300.00     |N  |  1.5813  | 20.2029   |
1518159|MACCARONE       |  1       |SWIFT BULGE SURVEY  |274.00     |N  |266.4168  |-29.0078   |
1518162|GELBORD         |  1       |MRK 876             |183.00     |N  |243.4882  | 65.7193   |
1518168|HOWELL          |  1       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          |  2       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          |  3       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          |  4       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          |  5       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          |  6       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          |  7       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          |  8       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          |  9       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 10       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 11       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 12       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 13       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 14       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 15       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 16       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 17       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 18       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 19       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 20       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 21       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 22       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 23       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 24       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 25       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 26       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 27       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 28       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 29       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 30       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 31       |HIGHEST URGENCY TARG|  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 32       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 33       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 34       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 35       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 36       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 37       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 38       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 39       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 40       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 41       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 42       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 43       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 44       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 45       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 46       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 47       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 48       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 49       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 50       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 51       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 52       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 53       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 54       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 55       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 56       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 57       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 58       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 59       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |
1518168|HOWELL          | 60       |HIGH URGENCY TARGET |  7.50     |Y  |  0.0000  |  0.0000   |

1518002|GRUPE           |  1       |ESO 242-G8          |  1.00     |N  |  6.2508  |-45.4928   |
1518002|GRUPE           |  2       |TON S 180           |  1.00     |N  | 14.3342  |-22.3825   |
1518002|GRUPE           |  3       |QSO 0056-36         |  1.00     |N  | 14.6558  |-36.1014   |
1518002|GRUPE           |  4       |RX J0100-5113       |  1.00     |N  | 15.1129  |-51.2317   |
1518002|GRUPE           |  5       |RX J0105.6-1416     |  1.00     |N  | 16.4117  |-14.2706   |
1518002|GRUPE           |  6       |RX J0117-3826       |  1.00     |N  | 19.3775  |-38.4417   |
1518002|GRUPE           |  7       |MS 0117-28          |  1.00     |N  | 19.8987  |-28.3589   |
1518002|GRUPE           |  8       |RX J0128.1-1848     |  1.00     |N  | 22.0279  |-18.8086   |
1518002|GRUPE           |  9       |IRAS F01267-217     |  1.00     |N  | 22.2946  |-21.6992   |
1518002|GRUPE           | 10       |RX J0134.2-4258     |  1.00     |N  | 23.5704  |-42.9742   |
1518002|GRUPE           | 11       |RX J0136.9-3510     |  1.00     |N  | 24.2267  |-35.1644   |
1518002|GRUPE           | 12       |RX J0148.3-2758     |  1.00     |N  | 27.0929  |-27.9739   |
1518002|GRUPE           | 13       |RX J0152.4-2319     |  1.00     |N  | 28.1129  |-23.3317   |
1518002|GRUPE           | 14       |MKN 1044            |  1.00     |N  | 37.5229  | -8.9981   |
1518002|GRUPE           | 15       |MKN 1048            |  1.00     |N  | 38.6575  | -8.7878   |
1518002|GRUPE           | 16       |RX J0311.3-2046     |  1.00     |N  | 47.8283  |-20.7719   |
1518002|GRUPE           | 17       |RX J0319.8-2627     |  1.00     |N  | 49.9529  |-26.4533   |
1518002|GRUPE           | 18       |RX J0323.2-4931     |  1.00     |N  | 50.8158  |-49.5197   |
1518002|GRUPE           | 19       |ESO 301-G13         |  1.00     |N  | 51.2604  |-41.9050   |
1518002|GRUPE           | 20       |VCV 0331-37         |  1.00     |N  | 53.4175  |-37.1153   |
1518002|GRUPE           | 21       |RX J0349.1-4711     |  1.00     |N  | 57.2821  |-47.1844   |
1518002|GRUPE           | 22       |FAIRALL 1116        |  1.00     |N  | 57.9237  |-40.4667   |
1518002|GRUPE           | 23       |FAIRALL 1119        |  1.00     |N  | 61.2571  |-37.1875   |
1518002|GRUPE           | 24       |RX J0412.7-4712     |  1.00     |N  | 63.1729  |-47.2128   |
1518002|GRUPE           | 25       |1H 0419-577         |  1.00     |N  | 66.2529  |-57.2006   |
1518002|GRUPE           | 26       |FAIRALL 303         |  1.00     |N  | 67.6667  |-53.6156   |
1518002|GRUPE           | 27       |RX J0437.4-4711     |  1.00     |N  | 69.3675  |-47.1917   |
1518002|GRUPE           | 28       |RX J0439.6-5311     |  1.00     |N  | 69.9112  |-53.1919   |
1518002|GRUPE           | 29       |1H 0439-272         |  1.00     |N  | 70.3438  |-27.1389   |
1518002|GRUPE           | 30       |1 ES 0614-584       |  1.00     |N  | 93.9567  |-58.4350   |
1518002|GRUPE           | 31       |RX J0859.0+4846     |  1.00     |N  |134.7621  | 48.7692   |
1518002|GRUPE           | 32       |RX J0902.5-0700     |  1.00     |N  |135.6400  | -7.0011   |
1518002|GRUPE           | 33       |MKN 110             |  1.00     |N  |141.3042  | 52.2867   |
1518002|GRUPE           | 34       |PG 0953+414         |  1.00     |N  |149.2183  | 41.2561   |
1518002|GRUPE           | 35       |RX J1005.7+4332     |  1.00     |N  |151.4246  | 43.5447   |
1518002|GRUPE           | 36       |RX J1007.1+2203     |  1.00     |N  |151.7925  | 22.0506   |
1518002|GRUPE           | 37       |CBS 126             |  1.00     |N  |153.2625  | 35.8567   |
1518002|GRUPE           | 38       |HS 1019+37          |  1.00     |N  |154.7521  | 37.8781   |
1518002|GRUPE           | 39       |MKN 141             |  1.00     |N  |154.8025  | 63.9675   |
1518002|GRUPE           | 40       |MKN 142             |  1.00     |N  |156.3804  | 51.6764   |
1518002|GRUPE           | 41       |RX J1034.6+3938     |  1.00     |N  |158.6608  | 39.6411   |
1518002|GRUPE           | 42       |RX J1117.1+6522     |  1.00     |N  |169.2921  | 65.3686   |
1518002|GRUPE           | 43       |PG 1115+407         |  1.00     |N  |169.6267  | 40.4319   |
1518002|GRUPE           | 44       |TON 1388            |  1.00     |N  |169.7862  | 21.3217   |
1518002|GRUPE           | 45       |EXO 1128+69         |  1.00     |N  |172.7700  | 68.8647   |
1518002|GRUPE           | 46       |2B 1128+31          |  1.00     |N  |172.7896  | 31.2350   |
1518002|GRUPE           | 47       |SBS 1136+579        |  1.00     |N  |174.7067  | 57.7122   |
1518002|GRUPE           | 48       |Z 1136+3412         |  1.00     |N  |174.8079  | 33.9308   |
1518002|GRUPE           | 49       |WAS 26              |  1.00     |N  |175.3175  | 21.9392   |
1518002|GRUPE           | 50       |CASG 855            |  1.00     |N  |176.1246  | 36.8858   |
1518002|GRUPE           | 51       |MKN 1310            |  1.00     |N  |180.3100  | -3.6781   |
1518002|GRUPE           | 52       |NGC 4051            |  1.00     |N  |180.7896  | 44.5306   |
1518002|GRUPE           | 53       |GQ COMAE            |  1.00     |N  |181.1754  | 27.9033   |
1518002|GRUPE           | 54       |RX J1209.8+3217     |  1.00     |N  |182.4383  | 32.2839   |
1518002|GRUPE           | 55       |PG 1211+143         |  1.00     |N  |183.5737  | 14.0536   |
1518002|GRUPE           | 56       |MKN 766             |  1.00     |N  |184.6108  | 29.8128   |
1518002|GRUPE           | 57       |3C 273              |  1.00     |N  |187.2779  |  2.0525   |
1518002|GRUPE           | 58       |RX J1231.6+7044     |  1.00     |N  |187.9025  | 70.7372   |
1518002|GRUPE           | 59       |MKN 771             |  1.00     |N  |188.0150  | 20.1583   |
1518002|GRUPE           | 60       |TON 83              |  1.00     |N  |188.4238  | 31.0175   |
1518002|GRUPE           | 61       |MCG+08-23-067       |  1.00     |N  |189.2133  | 45.6514   |
1518002|GRUPE           | 62       |NGC 4593            |  1.00     |N  |189.9142  | -5.3442   |
1518002|GRUPE           | 63       |IRAS F12397+3333    |  1.00     |N  |190.5442  | 33.2842   |
1518002|GRUPE           | 64       |PG 1244+026         |  1.00     |N  |191.6467  |  2.3692   |
1518002|GRUPE           | 65       |RX J1304.2+0205     |  1.00     |N  |196.0708  |  2.0936   |
1518002|GRUPE           | 66       |PG 1307+085         |  1.00     |N  |197.4458  |  8.3300   |
1518002|GRUPE           | 67       |RX J1314.3+3429     |  1.00     |N  |198.5946  | 34.4942   |
1518002|GRUPE           | 68       |RX J1319.9+5235     |  1.00     |N  |199.9879  | 52.5925   |
1518002|GRUPE           | 69       |PG 1322+659         |  1.00     |N  |200.9563  | 65.6967   |
1518002|GRUPE           | 70       |IRAS 13349+2438     |  1.00     |N  |204.3279  | 24.3842   |
1518002|GRUPE           | 71       |TON 730             |  1.00     |N  |205.9863  | 25.6467   |
1518002|GRUPE           | 72       |RX J1355.2+5612     |  1.00     |N  |208.8192  | 56.2125   |
1518002|GRUPE           | 73       |PG 1402+261         |  1.00     |N  |211.3175  | 25.9261   |
1518002|GRUPE           | 74       |RX J1413.6+7029     |  1.00     |N  |213.4029  | 70.4972   |
1518002|GRUPE           | 75       |NGC 5548            |  1.00     |N  |214.4958  | 25.1367   |
1518002|GRUPE           | 76       |QSO 1421-0013       |  1.00     |N  |216.0158  | -0.4494   |
1518002|GRUPE           | 77       |MKN 813             |  1.00     |N  |216.8542  | 19.8314   |
1518002|GRUPE           | 78       |MKN 684             |  1.00     |N  |217.7671  | 28.2872   |
1518002|GRUPE           | 79       |MKN 478             |  1.00     |N  |220.5312  | 35.4397   |
1518002|GRUPE           | 80       |PG 1448+273         |  1.00     |N  |222.7867  | 27.1575   |
1518002|GRUPE           | 81       |MKN 841             |  1.00     |N  |226.0050  | 10.4378   |
1518002|GRUPE           | 82       |SBS 1527+564        |  1.00     |N  |232.2812  | 56.2686   |
1518002|GRUPE           | 83       |MKN 493             |  1.00     |N  |239.7904  | 35.0300   |
1518002|GRUPE           | 84       |MKN 876             |  1.00     |N  |243.4883  | 65.7197   |
1518002|GRUPE           | 85       |RX J1618.1+3619     |  1.00     |N  |244.5392  | 36.3328   |
1518002|GRUPE           | 86       |KUG 1618+40         |  1.00     |N  |244.9638  | 40.9800   |
1518002|GRUPE           | 87       |PG 1626+554         |  1.00     |N  |246.9837  | 55.3756   |
1518002|GRUPE           | 88       |EXO 1627+4014       |  1.00     |N  |247.2554  | 40.1333   |
1518002|GRUPE           | 89       |RX J1702.5+3247     |  1.00     |N  |255.6296  | 32.7889   |
1518002|GRUPE           | 90       |II ZW 136           |  1.00     |N  |323.1162  | 10.1389   |
1518002|GRUPE           | 91       |RX J2146.6-3051     |  1.00     |N  |326.6500  |-30.8614   |
1518002|GRUPE           | 92       |ESO 404-G029        |  1.00     |N  |331.9375  |-32.5836   |
1518002|GRUPE           | 93       |NGC 7214            |  1.00     |N  |332.2792  |-27.8100   |
1518002|GRUPE           | 94       |RX J2216.8-4451     |  1.00     |N  |334.2217  |-44.8658   |
1518002|GRUPE           | 95       |RX J2217.9-5941     |  1.00     |N  |334.4858  |-59.6917   |
1518002|GRUPE           | 96       |PKS 2227-399        |  1.00     |N  |337.6679  |-39.7144   |
1518002|GRUPE           | 97       |RX J2242.6-3845     |  1.00     |N  |340.6571  |-38.7544   |
1518002|GRUPE           | 98       |RX J2245.2-4652     |  1.00     |N  |341.3346  |-46.8700   |
1518002|GRUPE           | 99       |MS 2254-36          |  1.00     |N  |344.4125  |-36.9353   |
1518002|GRUPE           |100       |RX J2258.7-2609     |  1.00     |N  |344.6892  |-26.1539   |
1518002|GRUPE           |101       |RX J2301.6-5913     |  1.00     |N  |345.4008  |-59.2222   |
1518002|GRUPE           |102       |RX J2301.8-5508     |  1.00     |N  |345.4667  |-55.1419   |
1518002|GRUPE           |103       |RX J2304.6-3501     |  1.00     |N  |346.1554  |-35.0203   |
1518002|GRUPE           |104       |RX J2312.5-3404     |  1.00     |N  |348.1450  |-34.0722   |
1518002|GRUPE           |105       |RX J2317.8-4422     |  1.00     |N  |349.4579  |-44.3744   |
1518002|GRUPE           |106       |RX J2325.2-3236     |  1.00     |N  |351.2992  |-32.6097   |
1518002|GRUPE           |107       |IRAS F23226-3843    |  1.00     |N  |351.3508  |-38.4469   |
1518002|GRUPE           |108       |MS 23409-1511       |  1.00     |N  |355.8692  |-14.9250   |
1518002|GRUPE           |109       |RX J2349.4-3126     |  1.00     |N  |357.3504  |-31.4342   |
1518002|GRUPE           |110       |AM 2354-304         |  1.00     |N  |359.3667  |-30.4611   |
1518022|KENNEA          |  1       |MAXI TRANSIENT #1   |  1.00     |Y  |  0.0000  |  0.0000   |
1518022|KENNEA          |  2       |MAXI TRANSIENT #2   |  1.00     |Y  |  0.0000  |  0.0000   |
1518022|KENNEA          |  3       |MAXI TRANSIENT #3   |  1.00     |Y  |  0.0000  |  0.0000   |
1518022|KENNEA          |  4       |MAXI TRANSIENT #4   |  2.00     |Y  |  0.0000  |  0.0000   |
1518022|KENNEA          |  5       |MAXI TRANSIENT #5   |  2.00     |Y  |  0.0000  |  0.0000   |
1518022|KENNEA          |  6       |MAXI TRANSIENT #6   |  3.50     |Y  |  0.0000  |  0.0000   |
1518022|KENNEA          |  7       |MAXI TRANSIENT #7   |  9.50     |Y  |  0.0000  |  0.0000   |
1518027|VAN DEN EIJNDEN |  1       |VFXT                | 30.00     |Y  |  0.0000  |  0.0000   |
1518033|BOGDANOV        |  1       |PSR J1023+0038      | 80.00     |Y  |155.9487  |  0.6448   |
1518033|BOGDANOV        |  2       |XSS J12270-4859     | 80.00     |Y  |186.9948  |-48.8952   |
1518033|BOGDANOV        |  3       |PSR J1723-2837      | 80.00     |Y  |260.8466  |-28.6325   |
1518033|BOGDANOV        |  4       |J1628-3205          | 80.00     |Y  |247.0292  |-32.0969   |
1518033|BOGDANOV        |  5       |PSR J2129-0429      | 80.00     |Y  |322.4375  | -4.4849   |
1518033|BOGDANOV        |  6       |PSR J1816+4510      | 80.00     |Y  |274.1497  | 45.1761   |
1518033|BOGDANOV        |  7       |PSR J2215+5135      | 80.00     |Y  |333.8862  | 51.5935   |
1518033|BOGDANOV        |  8       |PSR J2339-0533      | 80.00     |Y  |354.9115  | -5.5515   |
1518033|BOGDANOV        |  9       |1FGL J0523.5-2529   | 80.00     |Y  | 80.8205  |-25.4602   |
1518033|BOGDANOV        | 10       |PSR J1417-4402      | 80.00     |Y  |214.3775  |-44.0493   |
1518033|BOGDANOV        | 11       |3FGL J1544.6-1125   | 80.00     |Y  |236.1641  |-11.4679   |
1518033|BOGDANOV        | 12       |PSR J1048+2339      | 80.00     |Y  |162.1809  | 23.6648   |
1518033|BOGDANOV        | 13       |3FGL J0212.1+5320   | 80.00     |Y  | 33.0436  | 53.3607   |
1518033|BOGDANOV        | 14       |3FGL J0427-6704     | 80.00     |Y  | 66.9567  |-67.0764   |
1518033|BOGDANOV        | 15       |3FGL J0744.1-2523   | 80.00     |Y  |116.0353  |-25.3997   |
1518033|BOGDANOV        | 16       |3FGL J0838.8-2829   | 80.00     |Y  |129.7102  |-28.4659   |
1518033|BOGDANOV        | 17       |3FGL J2039.6-5618   | 80.00     |Y  |309.8958  |-56.2858   |
1518033|BOGDANOV        | 18       |NEW REDBACK         | 80.00     |Y  |  0.0000  |  0.0000   |
1518057|FUERST          |  1       |NGC 5907 ULX1       | 52.00     |N  |228.9957  | 56.3030   |
1518057|FUERST          |  2       |NGC 7793 P13        | 41.00     |N  |359.4625  |-32.6241   |
1518059|WARGELIN        |  1       |PROXIMA CEN         | 49.00     |N  |217.3838  |-62.6753   |
1518068|DEGENAAR        |  1       |TRANSIENT BEXRB     | 20.00     |Y  |  0.0000  |  0.0000   |
1518078|SAND            |  1       |DLT_1               | 36.00     |Y  |  0.0000  |  0.0000   |
1518078|SAND            |  2       |DLT_2               | 36.00     |Y  |  0.0000  |  0.0000   |
1518078|SAND            |  3       |DLT_3               | 36.00     |Y  |  0.0000  |  0.0000   |
1518078|SAND            |  4       |DLT_4               | 36.00     |Y  |  0.0000  |  0.0000   |
1518078|SAND            |  5       |DLT_5               | 36.00     |Y  |  0.0000  |  0.0000   |
1518089|SMITH           |  1       |3C 371              | 77.00     |N  |271.7112  | 69.8245   |
1518089|SMITH           |  2       |S4 1749+70          | 70.00     |N  |267.1368  | 70.0974   |
1518089|SMITH           |  3       |S5 1803+784         | 87.50     |N  |270.1903  | 78.4678   |
1518089|SMITH           |  4       |4C +56.27           | 87.50     |N  |276.0295  | 56.8504   |
1518099|URSINI          |  1       |4C 40.08            |  5.00     |N  | 30.1254  | 40.8147   |
1518099|URSINI          |  2       |LQAC 033+032 002    |  5.00     |N  | 33.5642  | 32.8514   |
1518099|URSINI          |  3       |NVSS J065426+731950 |  5.00     |N  |103.6112  | 73.3306   |
1518099|URSINI          |  4       |NVSS J065846+491249 |  5.00     |N  |104.6933  | 49.2067   |
1518099|URSINI          |  5       |4C 75.02A           |  5.00     |N  |124.9604  | 75.6444   |
1518099|URSINI          |  6       |NVSS J121158+741904 |  5.00     |N  |182.9946  | 74.3178   |
1518099|URSINI          |  7       |FBQS J1216+4159     |  5.00     |N  |184.0400  | 41.9911   |
1518099|URSINI          |  8       |B3 1309+412A        |  5.00     |N  |197.9296  | 40.9833   |
1518099|URSINI          |  9       |4C 69.15            |  5.00     |N  |198.4950  | 69.6217   |
1518099|URSINI          | 10       |B2 1358+30C         |  5.00     |N  |210.1808  | 30.3219   |
1518099|URSINI          | 11       |NVSS J142819+291845 |  5.00     |N  |217.0800  | 29.3122   |
1518099|URSINI          | 12       |4C 33.33            |  5.00     |N  |223.2621  | 33.1447   |
1518099|URSINI          | 13       |NVSS J153657+842310 |  5.00     |N  |234.2388  | 84.3864   |
1518099|URSINI          | 14       |B1918+516           |  5.00     |N  |289.8446  | 51.7261   |
1518100|AUCHETTL        |  1       |ASASSN-14LI         | 14.00     |N  |192.0633  | 17.7739   |
1518100|AUCHETTL        |  2       |ASASSN-15OI         | 25.00     |N  |309.7879  |-30.7557   |
1518100|AUCHETTL        |  3       |PS18KH              | 30.00     |N  |119.2271  | 34.2621   |
1518100|AUCHETTL        |  4       |ASASSN-18PG         | 30.00     |N  |242.7450  |-60.9231   |
1518100|AUCHETTL        |  5       |ASASSN-18UL         | 30.00     |N  |342.5673  |-44.8646   |
1518118|SAKAMOTO        |  1       |MAXI GRB1           |  7.00     |Y  |  0.0000  |  0.0000   |
1518118|SAKAMOTO        |  2       |MAXI GRB2           |  7.00     |Y  |  0.0000  |  0.0000   |
1518118|SAKAMOTO        |  3       |MAXI GRB3           |  7.00     |Y  |  0.0000  |  0.0000   |
1518118|SAKAMOTO        |  4       |MAXI GRB4           |  7.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      |  1       |FRB 1               |  2.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      |  2       |FRB 2               |  2.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      |  3       |FRB 3               |  2.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      |  4       |FRB 4               |  2.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      |  5       |FRB 5               |  2.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      |  6       |FRB 6               |  2.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      |  7       |FRB 7               |  2.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      |  8       |FRB 8               |  2.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      |  9       |FRB 9               |  2.00     |Y  |  0.0000  |  0.0000   |
1518131|TOHUVAVOHU      | 10       |FRB 10              |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       |  1       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       |  2       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       |  3       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       |  4       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       |  5       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       |  6       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       |  7       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       |  8       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       |  9       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       | 10       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       | 11       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       | 12       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       | 13       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       | 14       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       | 15       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518145|SANTANDER       | 16       |LATPHOTON           |  2.00     |Y  |  0.0000  |  0.0000   |
1518164|PALIYA          |  1       |2WHSP J0320-7045    |  5.00     |N  | 50.0379  |-70.7592   |
1518164|PALIYA          |  2       |2WHSP J0442+6140    |  3.00     |N  | 70.6692  | 61.6775   |
1518164|PALIYA          |  3       |2WHSP J0731+2804    |  5.00     |N  |112.9692  | 28.0756   |
1518164|PALIYA          |  4       |2WHSP J1123-3232    |  5.00     |N  |170.8246  |-32.5381   |
1518164|PALIYA          |  5       |2WHSP J1451+6354    |  5.00     |N  |222.8654  | 63.9053   |
1518164|PALIYA          |  6       |2WHSP J1606+5630    |  5.00     |N  |241.5867  | 56.5044   |
1518164|PALIYA          |  7       |2WHSP J1623+0857    |  5.00     |N  |245.8767  |  8.9567   |
1518164|PALIYA          |  8       |2WHSP J1904+3626    |  5.00     |N  |286.0492  | 36.4492   |
1518164|PALIYA          |  9       |2WHSP J2052+0810    |  5.00     |N  |313.1767  |  8.1778   |
1518164|PALIYA          | 10       |2WHSP J2233+1336    |  2.00     |N  |338.2542  | 13.6003   |
1518170|PASHAM          |  1       |HOLMBERG II X-1     | 25.00     |N  |124.8758  | 70.7050   |
1518170|PASHAM          |  2       |NGC 247 ULX         | 75.00     |N  | 11.7667  |-20.7956   |
1518177|MACGREGOR       |  1       |PROXIMA CENTAURI    | 90.00     |N  |217.4290  |-62.6795   |
1518185|KEIVANI         |  1       |GWHEN1 MOSAIC       |  9.50     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         |  2       |GWHEN2 MOSAIC       |  9.50     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         |  3       |GWHEN3 MOSAIC       |  9.50     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         |  4       |GWHEN4 MOSAIC       |  9.50     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         |  5       |GWHEN1 SOURCE A     |  2.00     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         |  6       |GWHEN1 SOURCE B     |  2.00     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         |  7       |GWHEN2 SOURCE A     |  2.00     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         |  8       |GWHEN2 SOURCE B     |  2.00     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         |  9       |GWHEN3 SOURCE A     |  2.00     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         | 10       |GWHEN3 SOURCE B     |  2.00     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         | 11       |GWHEN4 SOURCE A     |  2.00     |Y  |  0.0000  |  0.0000   |
1518185|KEIVANI         | 12       |GWHEN4 SOURCE B     |  2.00     |Y  |  0.0000  |  0.0000   |
1518186|TERRERAN        |  1       |SLSN1               |110.00     |Y  |  0.0000  |  0.0000   |
1518186|TERRERAN        |  2       |SLSN2               |110.00     |Y  |  0.0000  |  0.0000   |
1518191|AYALA SOLARES   |  1       |ANT_FERMI_ALERT     | 14.00     |Y  |  0.0000  |  0.0000   |
1518191|AYALA SOLARES   |  2       |ICECUBE_FERMI_ALERT | 14.00     |Y  |  0.0000  |  0.0000   |
1518191|AYALA SOLARES   |  3       |ICECUBE_HAWC_ALERT  | 15.00     |Y  |  0.0000  |  0.0000   |
1518191|AYALA SOLARES   |  4       |ICECUBE_SWIFTB_ALERT| 15.00     |Y  |  0.0000  |  0.0000   |
1518191|AYALA SOLARES   |  5       |COINCIDENCE SOURCE 1|  5.00     |Y  |  0.0000  |  0.0000   |
1518191|AYALA SOLARES   |  6       |COINCIDENCE SOURCE 2|  5.00     |Y  |  0.0000  |  0.0000   |
1518194|KUIN            |  1       |TDE1                | 15.00     |Y  |  0.0000  |  0.0000   |
1518199|HOMAN           |  1       |H1743-322           | 53.00     |N  |266.5650  |-32.2335   |
1518200|FOLEY           |  1       |TRANSIENT           |  9.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           |  2       |TRANSIENT           |  9.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           |  3       |TRANSIENT           |  9.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           |  4       |TRANSIENT           |  9.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           |  5       |TRANSIENT           |  9.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           |  6       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           |  7       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           |  8       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           |  9       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 10       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 11       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 12       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 13       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 14       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 15       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 16       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 17       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 18       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 19       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 20       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 21       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 22       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 23       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 24       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518200|FOLEY           | 25       |TRANSIENT           |  5.00     |Y  |  0.0000  |  0.0000   |
1518203|HENZE           |  1       |M31N 2008-12A       | 84.00     |Y  | 11.3704  | 41.9028   |
1518206|D'ORAZIO        |  1       |KIC 11606854        | 30.00     |N  |289.6899  | 49.6322   |
1518214|BROWN           |  1       |ANON-SN2018FEB      |  3.00     |N  |257.5465  | 21.6490   |
1518214|BROWN           |  2       |CGCG137-068-SN2018CO|  4.00     |N  |244.0009  | 22.2678   |
1518214|BROWN           |  3       |ANON-SN2018BTA      |  2.00     |N  |254.4948  |-62.7316   |
1518214|BROWN           |  4       |ANON-SN2018BGV      |  3.00     |N  |165.6262  | 55.5988   |
1518214|BROWN           |  5       |ANON-SN2018AVK      |  2.00     |N  |197.8656  | 65.6381   |
1518214|BROWN           |  6       |ANON-SN2018ATQ      |  2.00     |N  |176.7672  | 19.5508   |
1518214|BROWN           |  7       |ANON-ASASSN-18GQ    |  3.00     |N  |206.2645  |-41.8732   |
1518214|BROWN           |  8       |ANON-ASASSN-18GE    |  2.00     |N  |218.3330  | 41.2676   |
1518214|BROWN           |  9       |ANON-ASASSN-18AP    |  2.00     |N  | 26.6750  | 32.5075   |
1518214|BROWN           | 10       |ANON-SN2018ZD       |  2.00     |N  | 94.5132  | 78.3669   |
1518214|BROWN           | 11       |ANON-SN2018IS       |  2.00     |N  |199.2390  |-16.6179   |
1518214|BROWN           | 12       |ANON-SN2018GJ       |  2.00     |N  |248.0100  | 78.2114   |
1518214|BROWN           | 13       |ANON-SN2018AFM      |  4.00     |N  |119.8543  | 16.4265   |
1518214|BROWN           | 14       |ANON-SN2017JMK      |  4.00     |N  |348.6882  |  4.5306   |
1518214|BROWN           | 15       |ANON-2017JMK        |  4.00     |N  |348.6875  |  4.5306   |
1518214|BROWN           | 16       |ANON-SN2017JBJ      |  2.00     |N  | 12.0226  | -2.7896   |
1518214|BROWN           | 17       |ANON-2018IS         |  2.00     |N  |199.2375  |-16.6178   |
1518214|BROWN           | 18       |ANON-2018GJ         |  2.00     |N  |248.0083  | 78.2114   |
1518214|BROWN           | 19       |ANON-2017JBJ        |  2.00     |N  | 12.0208  | -2.7894   |
1518214|BROWN           | 20       |ANON-2017IVU        |  4.00     |N  |234.1375  | 16.6054   |
1518214|BROWN           | 21       |ANON-SN2017HBJ      |  2.00     |N  | 67.7820  |-63.3197   |
1518214|BROWN           | 22       |ANON-2016EZH        |  4.00     |N  | 29.5208  | -0.8728   |
1518214|BROWN           | 23       |ESO155-G036-2017GRY |  3.00     |N  | 52.0331  |-56.5783   |
1518214|BROWN           | 24       |NGC1343-SN2017GPN   |  2.00     |N  | 54.4386  | 72.5330   |
1518214|BROWN           | 25       |NGC2748-SN2017GKK   |  2.00     |N  |138.4364  | 76.4789   |
1518214|BROWN           | 26       |ESO317-32-SN2017GHS |  2.00     |N  |157.0091  |-42.1058   |
1518214|BROWN           | 27       |NGC1672-SN2017GAX   |  4.00     |N  | 71.4560  |-59.2451   |
1518214|BROWN           | 28       |2MASXJ20171114+58120|  4.00     |N  |304.2973  | 58.2025   |
1518214|BROWN           | 29       |ANON-SN2017FHM      |  2.00     |N  |323.8136  | -6.9745   |
1518214|BROWN           | 30       |ANON-ASASSN-17IP    |  4.00     |N  |134.5875  |-65.3636   |
1518214|BROWN           | 31       |ANON-SN2017FAA      |  2.00     |N  |199.7663  | -2.5127   |
1518214|BROWN           | 32       |ANON-SN2017EQX      |  2.00     |N  |336.7015  | 17.1479   |
1518214|BROWN           | 33       |ANON-SN2017ERR      |  2.00     |N  |167.8546  |  0.1163   |
1518214|BROWN           | 34       |ANON-SN2017ENS?     |  2.00     |N  |181.0390  | -1.9312   |
1518214|BROWN           | 35       |ANON-ASASSN-17HO    |  2.00     |N  |289.6975  |-84.6976   |
1518214|BROWN           | 36       |ESO-215-G-037-SN2017|  3.00     |N  |168.9073  |-48.7487   |
1518214|BROWN           | 37       |ESO092-G014-SN2017EN|  2.00     |N  |152.7170  |-66.6473   |
1518214|BROWN           | 38       |NGC3938-SN2017EIN   |  2.00     |N  |178.2219  | 44.1239   |
1518214|BROWN           | 39       |NGC6946-SN2017EAW   |  2.00     |N  |308.6843  | 60.1933   |
1518214|BROWN           | 40       |2MASXJ09033237-21200|  2.00     |N  |135.8854  |-21.3341   |
1518214|BROWN           | 41       |ANON-SN2017DWH      |  2.00     |N  |218.6789  | 31.4879   |
1518214|BROWN           | 42       |ANON-SN2017DCC      |  2.00     |N  |192.2704  |-12.2062   |
1518214|BROWN           | 43       |NGC4532-SN2017DES   |  2.00     |N  |188.5788  |  6.4742   |
1518214|BROWN           | 44       |UGC09113-SN2017DAU  |  2.00     |N  |213.5712  | 35.4287   |
1518214|BROWN           | 45       |ANON-ASASSN-17EM    |  2.00     |N  |255.7990  | 61.4573   |
1518214|BROWN           | 46       |NGC4779-SN2017CJB   |  2.00     |N  |193.4602  |  9.7049   |
1518214|BROWN           | 47       |ANON-SN2017CAK      |  2.00     |N  |229.8286  | 28.2290   |
1518214|BROWN           | 48       |ANON-SN2017CZW      |  2.00     |N  |213.6340  | -3.5554   |
1518214|BROWN           | 49       |ANON-SN2017BGU      |  3.00     |N  |253.9978  | 42.5600   |
1518214|BROWN           | 50       |ANON-SN2017ATI      |  2.00     |N  |147.4863  | 67.1832   |
1518214|BROWN           | 51       |NGC3318-SN2017AHN   |  2.00     |N  |159.3227  |-41.6181   |
1518214|BROWN           | 52       |ANON-SN2017IT       |  2.00     |N  | 92.6548  |-34.1410   |
1518214|BROWN           | 53       |NGC2242-SN2016JBU   |  2.00     |N  |114.1082  |-69.5487   |
1518214|BROWN           | 54       |MCG-01-39-005-SN2016|  2.00     |N  |230.8325  | -4.1554   |
1518214|BROWN           | 55       |IC 2151-SN2016IYZ   |  2.00     |N  | 88.1560  |-17.7869   |
1518214|BROWN           | 56       |ANON-SN2016IYD      |  2.00     |N  |114.2907  |-52.3178   |
1518214|BROWN           | 57       |GALEXASC J100418.99+|  2.00     |N  |151.0775  | 43.4248   |
1518214|BROWN           | 58       |ANON-SN2016IET      |  2.00     |N  |188.1375  | 27.1209   |
1518214|BROWN           | 59       |APMUKS(BJ) B211942.5|  2.00     |N  |320.6042  |-11.9486   |
1518214|BROWN           | 60       |NGC1532-SN2016IAE   |  2.00     |N  | 63.0230  |-32.8624   |
1518214|BROWN           | 61       |UGC4461-SN2016HRV   |  2.00     |N  |128.3418  | 52.5309   |
1518214|BROWN           | 62       |ANON-SN2016HGM      |  3.00     |N  | 20.5489  |  0.9521   |
1518214|BROWN           | 63       |GALEXASCJ002132.53-0|  2.00     |N  |  5.3856  | -5.9567   |
1518214|BROWN           | 64       |ESO344-G021-SN2016CV|  2.00     |N  |334.9558  |-40.6676   |
1518214|BROWN           | 65       |GALEXASC J072024.60+|  2.00     |N  |110.1012  | 32.8503   |
1518214|BROWN           | 66       |NGC1171-SN2016G     |  3.00     |N  | 45.9906  | 43.4010   |
1518215|MILNE           |  1       |FUTURE SN FIELD     |  2.00     |Y  |  0.0000  |  0.0000   |





Proposal Abstracts

1518037 / KARA / UNIVERSITY OF MARYLAND (COLLEGE PARK)

KEY PROJECT  "SIMULTANEOUS DISC AND CORONA REVERBERATION MAPPING IN AGN MRK 335"

Reverberation light echoes from optical up to hard X-rays have successfully mapped out the accretion flows of AGN from the broad line region down (BLR) to the innermost stable circular orbit (ISCO) of the black hole. In recent years, Swift has made a breakthrough in reverberation mapping, by measuring X-ray/UV/optical time lags that map out the accretion disc. Disc reverberation mapping has successfully been completed in 6 AGN, but the results seem to suggest a departure from the standard picture of a compact X-ray corona irradiating a Shakura & Sunyaev thin disc. These results appear in tension with X-ray reverberation mapping results of sub-Eddington AGN, which prefer a compact corona within 10 gravitational radii irradiating a disc that extends down to or near the ISCO. To resolve this tension, we request a 100-day Swift disc reverberation mapping campaign of the well-known and highly variable AGN Mrk 335, simultaneous with an extensive X-ray reverberation campaign by XMM-Newton. Such a widespread campaign across different wavebands and timescales has never been attempted, and is essential for understanding the connection between the accretion disc and the corona.

1518159 / MACCARONE / TEXAS TECH UNIVERSITY

KEY PROJECT  "THE SWIFT GALACTIC BULGE MONITORING SURVEY: SECOND 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.

1518162 / GELBORD / SPECTRAL SCIENCES INC.

KEY PROJECT  "INTENSIVE AGN DISK REVERBERATION MAPPING OF MRK 876 WITH SWIFT AND TESS"

Led by Swift, Intensive Disk Reverberation Mapping (IDRM) is providing new insights into the physics of active galactic nuclei (AGN) and strongly challenging the standard thin accretion disk/reprocessing model of AGN central engines. Mrk 876, which lies in the TESS continuous viewing zone, presents a unique opportunity to conduct a year-long IDRM campaign with Swift and TESS. Using the unprecedented detail of the TESS light curve to anchor the cross-correlation analysis will provide by far the strongest test of accretion disk structure to date. We request 366 500 s Swift pointings. These will be combined with TESS and ground-based griz data to perform echo mapping on the disk. Spectral monitoring will be used to disentangle contributions to the lags from the disk and broad-line region.

1518168 / HOWELL / LAS CUMBRES OBSERVATORY

KEY PROJECT  "MAXIMIZING SWIFT S IMPACT WITH THE GLOBAL SUPERNOVA PROJECT"

We request Swift UV photometry of 60 supernovae (SNe) over 2 years to be taken in conjunction with optical and IR data from the Global Supernova Project (GSP). The GSP is a 3 year key project led by Las Cumbres Observatory (LCO), involving 150+ members of the global community to obtain lightcurves and spectra of 500 SNe. With this data we will: (1) determine the progenitors of some SNe Ia; (2) probe the radius and structure of SN progenitors via shock cooling; (3) measure the UV flux in SNe where it is poorly known, including SNe Ib/c and fast transients; (4) probe the circumstellar material around some SNe Ia, and (5) create bolometric lightcurves for a large sample of SNe allowing better tests of theoretical models. The combined data set will be of lasting legacy value.

1518002 / GRUPE / MOREHEAD STATE UNIVERSITY

"CATCHING AGN IN EXTREME X-RAY FLUX STATES"

We propose to re-observe a sample of 110 X-ray bright AGN with Swift for 1 ks each in order to to identify least one of these AGN in an extreme X-ray flux state. This will then trigger our ongoing XMM/NuStar ToO program aiming to investigate in detail the X-ray spectra during extreme X-ray flux states and the drivers of their spectral complexity, including relativistically blurred reflection of X-ray photons off the accretion disk and extreme absorption events. The second goal of this proposal is to study the long-term variability of their SEDs and to study the physical conditions of extreme flux states allowing us to study how long-term variability affects important scaling relations in AGN, like correlations of AGN properties to understand the underlying physics.

1518022 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY

"SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS"

We propose to continue the highly successful program to use Swift to localize Galactic X-ray transients discovered by MAXI, the operational phase of which has been extended until March 31, 2021. 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.

1518027 / VAN DEN EIJNDEN / UNIVERSITEIT VAN AMSTERDAM

"THE NATURE AND ACCRETION FLOW PROPERTIES OF SUB-LUMINOUS X-RAY BINARIES"

Very-faint X-ray transients undergo outbursts of accretion with a peak X-ray luminosity much lower than that of other black hole and neutron star low-mass X-ray binaries. Studying these objects is of great interest because they trace a poorly understood accretion regime and may represent a missing population of short-period binaries or neutron stars with relatively strong magnetic fields. To study the outburst of a very-faint X-ray transient in detail, we propose 30 ks of Swift ToO monitoring observations (30x1 ks every other day), and 8h of deep VLA radio observations (2x4 hr). Complemented by guaranteed-time optical and near-infrared monitoring with Faulkes and SMARTS, these data allow us to investigate the nature of the binary and the properties of the accretion in/out flow.

1518033 / BOGDANOV / COLUMBIA UNIVERSITY

"OBSERVING THE NEXT X-RAY BINARY-RADIO MILLISECOND PULSAR TRANSITION"

In recent years, three millisecond pulsar binaries have been observed to switch between accreting and rotation-powered pulsar states, thereby unambiguously establishing the long-suspected link between low-mass X-ray binaries and "recycled" pulsars. In the accreting state, they exhibit X-ray and optical variability unlike anything observed in other X-ray binaries. We propose a continuation of our Swift XRT/UVOT target of opportunity program approved in Cycles 10, 11, and 13 to observe the next nearby binary recycled pulsar transformation to an accreting state. This will result in an improved understanding of the peculiar phenomenology of these systems, which may shed light on the little-understood physics of the quiescent regime in neutron star X-ray binaries.

1518057 / FUERST / EUROPEAN SPACE ASTRONOMY CENTRE (ESAC)

"SWIFT MONITORING OF NEUTRON STAR POWERED ULTRA-LUMINOUS X-RAY SOURCES"

We now know that some of the most luminous ultraluminous X-ray sources (ULXs) are powered by highly super-Eddington neutron star accretors. At least five such systems exist, with M82 X-2, NGC 7793 P13, and NGC 5907 ULX1 being the brightest ones, reaching luminosities over 1e40 erg/s. Here we propose to continue our successful Swift monitoring program performed in the last AOs of the latter two of these systems. NGC7793 P13 and NGC 5907 ULX1 are sufficiently isolated for Swift to provide robust fluxes, across the full visibility window available for each source in the upcoming cycle. These observations will probe the known super-orbital and orbital periods of these systems, measure the duty cycle of unusual off -states, and provide trigger criteria for follow-up observations.

1518059 / WARGELIN / SMITHSONIAN ASTROPHYSICAL OBSERVATORY

"PROXIMA CENTAURI'S STELLAR CYCLE"

Fifteen years of V-band monitoring have established the existence of a solar-like 7-year stellar cycle in Proxima Cen, a fully convective dM5.5e star, with further support from Swift X-ray and UV observations spanning a full cycle. This important discovery, along with related theoretical and observational work on fully convective stars in very recent years, is leading to major advances in our understanding of the structure and evolution of late M stars, and of cool-star magnetic fields in general. We request fourteen 3.5-ks observations with 12-day spacing to continue our long term study of the X-ray cycle. Prox Cen is the only late-type M star practical for such studies and Swift is uniquely well suited for the challenges of X-ray monitoring of this flare star.

1518068 / DEGENAAR / UNIVERSITEIT VAN AMSTERDAM

"SWIFT/VLA MONITORING OF THE DECAY OF A GIANT BE/X-RAY BINARY OUTBURST"

Our recent discovery of a radio jet produced by a highly magnetized neutron star in a Be/X-ray binary (BeXRB) has opened up an unexplored parameter regime to study the launching conditions of jets, and provides a novel avenue to complement existing X-ray studies to better understand the accretion flow in BeXRBs. We propose 20 ks Swift monitoring and 6 hr VLA time to study the decay of a giant outburst of a BeXRB. Our aims are to i) determine if a sharp transition in the 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 radio behavior in this regime. The proposed Swift observations will provide a rich data set that is highly valuable for the broader scientific community.

1518078 / SAND / UNIVERSITY OF ARIZONA

"HIGH CADENCE UV LIGHT CURVES OF EXTREMELY YOUNG SUPERNOVAE"

We are conducting a 12-hour cadence SN search of nearby galaxies (D<40 Mpc), directly tied to ground-based imaging/spectroscopy for immediate followup. In several instances, DLT40 and its ground-based follow-up have revealed early light curve features (which vary on hour time scales) that point to shock breakout, CSM or companion star interactions. One of the main limitations is the cadence of the accompanying Swift UV observations, which start 1-2-days after the request, and have typical cadences of 1 day. Here we request early, high cadence (6 hours) UV light curves of all young DLT40 SNe which have nondetections within 24 hours of discovery. This legacy dataset of 5 SNe, when combined with our ground-based campaigns, will point to the progenitor system and its environment.

1518089 / SMITH / STANFORD UNIVERSITY

"THE MISSING PIECE OF THE PUZZLE: SWIFT MONITORING OF TESS-FERMI BLAZARS"

Although multi-wavelength monitoring of the strongly variable emission of blazars has provided insights into high energy jet phenomena, one major mystery persists: the origin of the X-ray emission. Comparison between wavebands has been hampered in the past due to the sparse sampling and relatively poor photometric precision of ground-based optical timing. We plan to use the newly-launched exoplanet hunter TESS to obtain a cutting-edge sample of optical blazar light curves, leveraging our past success with Kepler. We propose for Swift to provide the critical simultaneous X-ray monitoring of four Fermi blazars to complement radio, optical, and gamma ray light curves and provide unprecedented insight into the physical connections and phenomenologies within relativistic jets.

1518099 / URSINI / INAF-OAS BOLOGNA

"TOWARDS A CENSUS OF THE ENERGETICS AND DUTY CYCLE OF GIANT RADIO GALAXIES"

We propose to observe 14 giant radio galaxies for the first time in the X-ray band. These sources are part of a complete sample of 26 giants selected from the WENSS 325-MHz radio survey. These new proposed observations will permit to constrain the X-ray flux of the sources and to compare their X-ray luminosities with the radio luminosities of the core and of the extended lobes. This will significantly extend our recent study of giant radio galaxies selected in the hard X-rays, by sampling a new region of the radio/X-ray luminosity parameter space. This will in turn constrain the duty cycle of the AGN/jet activity in a statistically significant sample of giant radio galaxies.

1518100 / AUCHETTL / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)

"LATE TIME MONITORING OF BRIGHT AND NEARBY OPTICAL TDES"

Dormant BHs at the centres of quiescent galaxies reveal themselves through luminous, accretion-powered flares called tidal disruption event (TDEs). These rare events provide us with unique insights into the physics associated with accretion and the BH itself. For most events, observations focus on the initial detection and follow-up of the flare. However, studies of the late time emission have revealed some surprises, indicating that TDEs undergo significant changes in their accretion and emission mechanisms as they evolve. But without detailed monitoring of this late time emission the uncertainties in this evolution is quite large. Here we propose to take advantage of Swift’s multi-wavelength capabilities to monitor the late time emission from some of the brightest/closest TDEs.

1518118 / SAKAMOTO / AOYAMA GAKUIN UNIVERSITY

"SWIFT RAPID FOLLOW-UP OBSERVATIONS OF MAXI XRFS AND LLGRBS"

We propose a Swift ToO program to observe XRFs and LLGRBs detected by MAXI to identify an afterglow with the Swift NFI instruments and the 105 cm Kiso wide field optical telescope. Our proposed "faster and better" GRB position from MAXI should enhance the afterglow detection of XRFs and LLGRBs. Since both XRFs and LLGRBs are extremely rare events, they are strong candidate sources for neutrino emission. We request a maximum of 4 ToOs in 7 tiling-mode observation (1 ks per tiling) to search for an X-ray afterglow candidate for the MAXI XRFs and LLGRBs.

1518131 / TOHUVAVOHU / THE PENNSYLVANIA STATE UNIVERSITY

"RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS"

We seek to quickly identify possible counterpart candidates to Fast Radio Bursts. To date no clear counterpart has been detected at non-radio wavelengths, and the progenitor systems and emission mechanism remain unknown. New abilities to detect and report Fast Radio Bursts in real time have been developed. We propose extremely rapid response follow-up observations with XRT and UVOT. We also propose to save the contemporaneous BAT event-by-event data when the FRB position is within the BAT FOV. We will utilize new enhancements to Swift’s fast-response capability to search for a counterpart in hard and soft X-rays and UV/Optical. This program will significantly enhance the science return of the Swift mission, and extend its transient response to help solve the mystery of Fast Radio Bursts.

1518145 / SANTANDER / UNIVERSITY OF ALABAMA

"PINPOINTING THE SOURCES OF 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. In this proposal we outline a program to perform ToO observations of single high-energy photons observed by Fermi-LAT with Swift XRT/UVOT to identify and characterize their sources. A detailed knowledge of the source populations that contribute to the overall observed isotropic gamma-ray flux is of key importance to understand the density and evolution of these sources with redshift, set constraints on a potential dark matter contribution, and study the link between the Isotropic Gamma-Ray Background (IGRB) and other cosmic backgrounds such as the diffuse neutrino flux discovered by the IceCube observatory.

1518164 / PALIYA / CLEMSON UNIVERSITY

"THE QUEST FOR THE MOST EFFICIENT PARTICLE ACCELERATORS"

We propose to carry out 2-5 ksec UVOT and XRT observations of ten extremely high synchrotron peaked (EHSP) BL Lacs whose synchrotron peak is expected to lie in the 0.3-10 keV energy band. These are some of the X-ray brightest EHSPs known so-far, however, lack X-ray spectral measurements. Our goal is to obtain the broadest simultaneous coverage from NIR to X-rays of the synchrotron spectrum to constrain the high-energy electron population. We will perform a detailed theoretical modeling to investigate the spectral shape of the electron population which is expected to be very hard. The fact that the same particles also radiates at GeV-TeV energies, the proposed sources are some of the most promising targets for the upcoming CTA and will be useful to explore the still poorly known EBL.

1518170 / PASHAM / MASSACHUSETTS INSTITUTE OF TECHNOLOGY

"HIGH-CADENCE XRT MONITORING OF ULTRALUMINOUS X-RAY SOURCES TO SEARCH FOR ORBITAL PERIODS"

Following the successful discovery of a 1.2 d period from high-cadence Swift monitoring of the ultraluminous X-ray source (ULX) in NGC 55 we propose similar monitoring observations (0.5ks and 1.5ksx5 visits per day for 10 days) of two more variable ULXs with known optical counterparts (Holmberg II X-1 and NGC 247 ULX). Our goal is to search for orbital periods in the range of a few 10s of hours in these sources. This particular period range--typical of stellar-mass black hole binaries--has rarely been probed before for ULXs. Any detected periods will be an important step towards dynamical mass measurement of these objects. With NGC 55 ULX we have already demonstrated that Swift, with its excellent X-ray sensitivity and fast maneuvering capability, can definitely perform these observations.

1518177 / MACGREGOR / CARNEGIE INSTITUTION OF WASHINGTON

"THE ORIGIN AND IMPACT OF FLARES IN THE PROXIMA CENTAURI PLANETARY SYSTEM"

At a distance of only 1.3 pc, Proxima Cen is the closest extrasolar planetary system and well-known as a flare star, making it a benchmark case to explore the potential effects of variability on the planet’s properties. Following our detection of a large mm flare, we have been awarded 36 hours of ALMA observations to monitor Proxima Cen in 2019. We propose to obtain simultaneous UV/X-ray coverage with Swift in order to (1) better constrain the properties of detected flares and their potential impact on planetary habitability, and (2) determine how stellar flaring emission correlates across the electromagnetic spectrum. By undertaking this comprehensive, multi-wavelength monitoring campaign of Proxima Cen, we will execute the first truly panchromatic analysis of M dwarf flaring activity.

1518180 / HAGEN / SPACE TELESCOPE SCIENCE INSTITUTE

"ENHANCING THE UVOT LEGACY: ENABLING EXTENDED SOURCE PHOTOMETRY"

The Swift Observations of the Local Volume (SOLV) survey is a Swift Team Key Project to image 465 galaxies in the Local Volume (d < 11 Mpc), spanning a representative range of morphologies, masses, and star formation histories. When combined with a rich archive of UV-to-IR imaging, UVOT provides the crucial multi-wavelength UV data needed to constrain the UV attenuation curve shape. However, UVOT has imaging artifacts that remain unquantified. While these have little effect on point sources, they are significant when performing extended source photometry. We propose to quantify these artifacts, which will enable analysis of the SOLV galaxies, as well as other existing and future observations of extended sources. The full analysis software package will be made available to the community.

1518185 / KEIVANI / COLUMBIA UNIVERSITY

"SEARCHING FOR X-RAY AND UV/O COUNTERPARTS OF GRAVITATIONAL WAVE AND HIGH-ENERGY NEUTRINO COINCIDENT SIGNALS WITH SWIFT"

We propose prompt searches for X-ray and UV/optical counterparts to gravitational wave (GW) and high-energy neutrino (HEN) coincident events with Swift. Using low-threshold GWs detected by LIGO/Virgo and low-threshold HENs detected by IceCube, we will perform a realtime coincidence search using our pipeline developed at Columbia University and select well-localized events with high correlation significances and high probabilities of cosmic origin. We set the selection criteria such that we request four triggers during Cycle 15. With the < 1 deg angular resolution of IceCube HENs, our triggers will prompt a 19-pointing mosaic by Swift, providing a significant coverage of the correlated event localization to 500 s depth in < 11 hour.

1518186 / TERRERAN / NORTHWESTERN UNIVERSITY

"EXPLOSION MECHANISMS AND ENERGY SOURCES POWERING SUPER-LUMINOUS SUPERNOVAE"

With peak luminosities L peak~10^45 erg/s, the new class of Super-Luminous supernovae (SLSNe) outshine standard SN explosions of a factor ~10-100 and represent the death of the most massive stars in our Universe. The nature of their exceptional luminosity is still unclear and requires exotic explosion mechanisms and/or peculiar sources of energy. Here we propose rapid Swift follow up of 2 newly-discovered SLSNe to map their UV and X-ray emission during the early stages of their evolution as part of our multi-wavelength effort through programs on the VLA, Chandra and optical/NIR facilities. The final aim is to: (i) Pin down the energy source of SLSNe; (ii) Map the diversity of their progenitor stars and pre-explosion evolution.

1518191 AYALA SOLARES / THE PENNSYLVANIA STATE UNIVERSITY

"SWIFT FOLLOW-UP SEARCHES OF LOW FALSE ALARM RATE HIGH-ENERGY NEUTRINO + GAMMA-RAY COINCIDENCES"

We request a set of four Swift ToO campaigns to search for X-ray and/or UV/optical counterparts to low false alarm rate multimessenger neutrino + gamma-ray coincidences during Cycle 15. We will be monitoring four distinct channels for such coincidences, and will trigger on any with false alarm rates, computed using scrambled datasets, of less than 1/yr. The AMON neutrino + gamma-ray alerts will be the first bona fide near real-time neutrino + gamma-ray alerts. The proposed Swift observations thus offer a new opportunity to discover neutrino + gamma-ray emitting sources within the subthreshold regime of the triggering observatories.

1518194 / KUIN / UNIVERSITY COLLEGE LONDON

"SWIFT ULTRAVIOLET SPECTROSCOPY OF TDE"

We propose a Swift UV grism spectroscopic follow-up of a UV-bright tidal disruption event (TDE) which will addultraviolet-optical coverage in the 1700-4500 ̊A band as well as observe any X-ray emission with the XRT. For low-redshift TDE, from the UV spectra we will be able to measure the 2175 ̊A reddening feature, and from the spectralline we can obtain an estimate of outflow velocities and from the uv spectral lines of C, N, O, and Mg obtain theexcitation/ionisation state in the debris. A series of observations will allow us to study the development of the debrisemission which can help constrain the TDE parameters.

1518199 / HOMAN / EUREKA SCIENTIFIC INC.

"A RARE LOOK AT A BLACK HOLE TRANSIENT EMERGING FROM QUIESCENCE"

The early phases of black hole transient outbursts are typically not well covered, due to the unpredictability of outbursts and the limited sensitivity of all-sky-monitors. We propose a ~3-month Swift monitoring campaign to catch the rise of the next outburst of the black hole transient H1743-322. The regularity of its outbursts provides us with a rare opportunity to follow a transient as it emerges from quiescence. Our X-ray observations will complement near-IR monitoring and we request additional VLA observations during the outburst rise. The goals of this campaign are to provide input to outburst disk-instability models and to study disk-jet coupling during outburst rise. We request a maximum of 53 (1 ks) Swift observations and 5 hrs of VLA time.

1518200 / FOLEY / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)

"YOUNG SUPERNOVA EXPERIMENT"

Observations of supernovae (SNe) within hours of explosion provide unique data about the exploding star, its circumstellar environment, and companions. Swift observations can look into a rare window where we see the system before and while the SN overruns its circumstellar material and companion. In particular, X-ray and UV observations probe the interaction between a SN and nearby gas/companion stars. The 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. With a new transient survey, the Young Supernova Experiment, we will identify dozens of SNe within hours of explosion, dramatically increasing the number of such SNe.

1518203 / HENZE / SAN DIEGO STATE UNIVERSITY

"PROBING THE ERUPTION STATISTICS AND EVOLUTION OF THE UNIQUE RECURRENT NOVA M31N 2008-12A"

M31N 2008-12a is a recurrent nova in M31 with a unique record of 10 observed eruptions in 10 years. Its ultra-short recurrence period presents the only opportunity to study a statistically significant number of eruptions from the same system. We propose a tailored 84-ks Swift X-ray/UV observing campaign of the predicted 2019 eruption as an integral part of a long-term project. The recent 2016 eruption deviated clearly from the previous pattern, underlining the importance of obtaining multi-eruption statistics. This benchmark data set will provide unparalleled insights into binary evolution and the eruption physics that determine the observable parameters. M31N 2008-12a remains the prime candidate for the progenitor of a type Ia supernova or an accretion induced collapse to a neutron star.

1518206 / D'ORAZIO / HARVARD-SMITHSONIAN CENTER FOR ASTROPHYSICS

"FIRST X-RAY OBSERVATIONS OF A PECULIAR FLARING AGN OBSERVED BY KEPLER: A SUPERMASSIVE BLACK HOLE BINARY HYPOTHESIS"

The Kepler-observed AGN KIC 11606854 exhibits a sawtooth-like oscillation over four years with a 10-day-duration symmetric flare at the center of the steep rising portion of this oscillation. This lightcurve can be exquisitely, and uniquely, modeled by gravitationally self-lensed and Doppler-boosted emission from an accreting supermassive black hole binary (SBHB) at the heart of KIC 11606854. Furthermore, the SBHB hypothesis predicts a unique, periodically repeating signature that can be tested on year timescales. As the Doppler boost scenario requires multi-wavelength data to confirm, and as lensing is most prominent in the X-ray, we propose for Swift XRT observations to determine the X-ray flux and spectral slope of this bright AGN before the date of the next predicted flare.

1518214 / BROWN / TEXAS A&M UNIVERSITY

"NOT DONE YET: TEMPLATE OBSERVATIONS TO COMPLETE SWIFT SUPERNOVAE"

The Swift Ultra-Violet/Optical Telescope (UVOT) has revolutionized the understanding of supernova (SN) behavior in the ultraviolet (UV). Swift has observed over 600 SNe, including examples of all major classes and most subtypes. This has enabled detailed studies of individual objects and to discover differences within SN subgroups. These studies relied on having the best possible photometric precision. Much of the original SN photometry is contaminated by the underlying host galaxy light. We propose reobserving the host galaxies of 66 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.

1518215 / MILNE / UNIVERSITY OF ARIZONA

"UVOT CALIBRATION OF TYPE IA SUPERNOVA FIELDS: \\ SEARCHING FOR GROUND-BASED EVIDENCE OF BI-MODALITY"

The UVOT instrument has been used to discover that there is a bi-modal distribution of the NUV-OPT colors of the normal type Ia supernovae that are used as cosmological distance indicators. This bi-modality has also been seen in spectrophotometry of high-z SNeIa, but with the group that is the minority group as low-z becoming the dominant group at high-z, which is of concern for the cosmological use of SNe~Ia. We request UVOT ubv observations of the fields of normal SNe~Ia that { bf will not be} observed with UVOT, but with the 1.5m-Kuiper-M4K camera. These observations will be used to calibrate the fields of these SNe on the UVOT~ubv system, so this sample can be compared to a control sample of SNe~Ia observed by both UVOT and the M4K . One ubv series of images are requested for 30 SNe Ia during this cycle in what will be a multi-cycle effort.