# Swift Cycle 17 Results

The lists below contain the proposals recommended by the Cycle 17 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 17 proposals for observation: Please note that the ROSES 2020 Appendix D.5 "Swift Guest Investigator Cycle 17" 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 17 ToO proposals may be triggered until March 31, 2022."

• To notify the Swift team that your trigger has occured, please use the Swift ToO web site and don't forget to use the proposal number for your proposal (below) when filling out the form.

## Recommended Proposals

Prop     PI                 Title

1720002  BOGDANOV           SWIFT MONITORING OF NEARBY X-RAY BINARY-RADIO MILLISECOND PULSAR TRANSITION OBJECTS
1720004  KENNEA             SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS
1720006  GAIDOS             X-RAYING THE INNER DISK OF A "DIPPER" STAR WITH SWIFT
1720020  MACCARONE          THE SWIFT GALACTIC BULGE MONITORING SURVEY: THIRD EPOCH
1720030  KENNEA             RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS
1720038  GRUPE              CATCHING AGN IN EXTREME X-RAY AND UV FLUX STATES
1720039  GRONWALL           DEEP UVOT IMAGING OF GOODS-NORTH
1720040  KRUMPE             EROSITA FOLLOW-UP OF RARE AGN IGNITIONS AND SHUT-DOWN EVENTS
1720041  FANG               DIAGNOSE THE GAMMA-RAY EMISSION MECHANISM OF THE CYGNUS COCOON WITH SWIFT-XRT
1720044  LIU                SWIFT REVERBERATION MAPPING OF A SUPERMASSIVE BLACK HOLE BINARY CANDIDATE
1720046  SICILIAN           CONSTRAINING THE STERILE NEUTRINO DARK MATTER PARAMETER SPACE WITH ARCHIVAL SWIFT DATA
1720050  DURBAK             RIMAS: THE RAPID IMAGER AND SPECTROGRAPH; A NEW TOOL FOR HIGH-REDSHIFT GRBS
1720061  MCHARDY            REVERBERATION MAPPING OF THE HIGH ACCRETION RATE AGN MCG+08-11-11
1720065  CHERNYAKOVA        SWIFT OBSERVATIONS OF PSR B1259-63 DURING ITS 2021 PERIASTRON PASSAGE
1720066  HOMAN              OBSERVING THE EARLY RISE OF X-RAY TRANSIENTS WITH SWIFT
1720067  WALTON             TESTING THE LENSE-THIRRING MODEL FOR ULX VARIABILITY WITH NGC5907 ULX1
1720084  CACKETT            AGN REVERBERATION MAPPING OF GAS FLOWS IN MRK 817 WITH SWIFT AND HUBBLE
1720090  DARNLEY            PROBING THE ERUPTION STATISTICS AND EVOLUTION OF THE UNIQUE RECURRENT NOVA M31N 2008-12A
1720095  AJELLO             TOWARDS THE FULL IDENTIFICATION OF THE 3FHL CATALOG
1720097  YOUNES             SWIFT X-RAY MONITORING OF THE MAGNETAR SGR 0755-2933
1720100  TORRES-ALBA        PROBING THE STRUCTURE OF THE AGN TORUS WITH SWIFT
1720105  CORSI              A SEARCH FOR BL-IC SNE WITH X-RAY AFTERGLOWS USING ZTF+SWIFT
1720111  JENCSON            HIGH-CADENCE UV LIGHT CURVES OF EXTREMELY YOUNG SUPERNOVAE
1720112  RAJAGOPAL          HUNTING HIGH REDSHIFT BLAZARS WITH SWIFT AND SARA-CT/ORM
1720117  HUNG               EARLY UV AND X-RAY EVOLUTION OF TIDAL DISRUPTION EVENTS IN YSE
1720118  HERVET             DAILY MONITORING OF MRK 421 FOR AN UNPRECEDENTED MULTI-WAVELENGTH VARIABILITY STUDY
1720122  LOPEZ NAVAS        MULTI WAVELENGTH MONITORING OF A CHANGING-LOOK PHENOMENON
1720126  DONAHUE            A NEW METHOD TO OBTAIN BLACK HOLE SPIN VALUES WITH 27 LOCAL AGN
1720128  HERVET             TOWARD A CONFIRMATION OF MULTIPLE RECOLLIMATION SHOCKS IN THE BL LAC MRK 421
1720132  HOMAN              INVESTIGATING SHALLOW HEATING IN NEUTRON STAR CRUSTS
1720137  MARGUTTI           A FOCUSED SWIFT INVESTIGATION OF FAST BLUE OPTICAL TRANSIENTS
1720139  AUCHETTL           THE FINAL STAGES OF BRIGHT OPTICAL TDES
1720141  MILLER             A SWIFT RESPONSE TO THERMONUCLEAR EXPLOSIONS
1720147  PASHAM             TRACKING THE LONG-TERM EVOLUTION OF QUASI-PERIODIC ERUPTIONS FROM A NEWLY DISCOVERED EROSITA
AGN USING XRT AND UVOT
1720150  MARSCHER           MONITORING IXPE BLAZAR TARGETS WITH SWIFT
1720152  SAKAMOTO           SWIFT RAPID FOLLOW-UP OBSERVATIONS OF MAXI XRFS AND LLGRBS
1720156  TERRERAN           EXPLOSION MECHANISMS AND ENERGY SOURCES POWERING SUPER-LUMINOUS SUPERNOVAE
1720157  CHORNOCK           DETAILED MAPPING OF EXTREME MASS-LOSS FROM EVOLVED MASSIVE STARS WITH SWIFT
1720161  WARGELIN           DOES PROXIMA CENTAURI REALLY HAVE A STELLAR CYCLE?
1720170  MCCARRIE           SHORT GRBS IN CLUSTERS OF GALAXIES
1720171  MOCKLER            MOSFIT: CONNECTING MODELS TO TIDAL DISRUPTION EVENT OBSERVATIONS
1720173  TRUMP              BLACK HOLE SPIN FROM CONTEMPORANEOUS UV-OPTICAL SEDS
1720180  SANTANDER          PROBING THE NEUTRINO-BLAZAR CONNECTION WITH SWIFT
1720183  BODEWITS           CHARACTERIZING THE DISTANT ACTIVITY EVOLUTION OF COMET C/2017 K2 (PANSTARRS)


## 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 ] |

1720002 | BOGDANOV    | 1          | PSR J1023+0038       | 4           | N   | 155.94871  | 0.64475     |
1720002 | BOGDANOV    | 2          | XSS J12270-4859      | 4           | N   | 186.99475  | -48.89522   |
1720002 | BOGDANOV    | 3          | PSR J1723-2837       | 4           | N   | 260.84658  | -28.63253   |
1720002 | BOGDANOV    | 4          | PSR J1628-3205       | 4           | N   | 247.02925  | -32.09686   |
1720002 | BOGDANOV    | 5          | PSR J2129-0429       | 4           | N   | 322.4375   | -4.48489    |
1720002 | BOGDANOV    | 6          | PSR J1816+4510       | 4           | N   | 274.14971  | 45.17608    |
1720002 | BOGDANOV    | 7          | PSR J2215+5135       | 4           | N   | 333.88617  | 51.59347    |
1720002 | BOGDANOV    | 8          | PSR J2339-0533       | 4           | N   | 354.91146  | -5.55147    |
1720002 | BOGDANOV    | 9          | 1FGL J0523.5-2529    | 4           | N   | 80.8205    | -25.46025   |
1720002 | BOGDANOV    | 10         | PSR J1417-4402       | 4           | N   | 214.3775   | -44.04925   |
1720002 | BOGDANOV    | 11         | 3FGL J1544.6-1125    | 4           | N   | 236.16408  | -11.46786   |
1720002 | BOGDANOV    | 12         | 3FGL J0427.9-6704    | 4           | N   | 66.95671   | -67.07639   |
1720002 | BOGDANOV    | 13         | PSR J1048+2339       | 4           | N   | 162.18088  | 23.66483    |
1720002 | BOGDANOV    | 14         | 3FGL J0212.1+5320    | 4           | N   | 33.04358   | 53.336      |
1720002 | BOGDANOV    | 15         | 3FGL J0744.1-2523    | 4           | N   | 116.03529  | -25.39969   |
1720002 | BOGDANOV    | 16         | 3FGL J0838.8-2829    | 4           | N   | 129.71021  | -28.46594   |
1720002 | BOGDANOV    | 17         | 3FGL J2039.6-5618    | 4           | N   | 309.89579  | -56.28583   |
1720004 | KENNEA      | 1          | MAXI TRANSIENT #1    | 1           | Y   | 0          | 0           |
1720004 | KENNEA      | 2          | MAXI TRANSIENT #2    | 1           | Y   | 0          | 0           |
1720004 | KENNEA      | 3          | MAXI TRANSIENT #3    | 1           | Y   | 0          | 0           |
1720004 | KENNEA      | 4          | MAXI TRANSIENT #4    | 1           | Y   | 0          | 0           |
1720004 | KENNEA      | 5          | MAXI TRANSIENT #5    | 2           | Y   | 0          | 0           |
1720004 | KENNEA      | 6          | MAXI TRANSIENT #6    | 2           | Y   | 0          | 0           |
1720004 | KENNEA      | 7          | MAXI TRANSIENT #7    | 3.5         | Y   | 0          | 0           |
1720006 | GAIDOS      | 1          | EP CHAMAELEONTIS     | 32          | N   | 131.75683  | -78.99289   |
1720020 | MACCARONE   | 1          | SWIFT BULGE SURVEY   | 274         | N   | 266.41683  | -29.00783   |
1720030 | KENNEA      | 1          | FRB 1                | 2           | Y   | 0          | 0           |
1720030 | KENNEA      | 2          | FRB 2                | 2           | Y   | 0          | 0           |
1720030 | KENNEA      | 3          | FRB 3                | 2           | Y   | 0          | 0           |
1720030 | KENNEA      | 4          | FRB 4                | 2           | Y   | 0          | 0           |
1720030 | KENNEA      | 5          | FRB 5                | 2           | Y   | 0          | 0           |
1720030 | KENNEA      | 6          | FRB 6                | 2           | Y   | 0          | 0           |
1720030 | KENNEA      | 7          | FRB 7                | 2           | Y   | 0          | 0           |
1720030 | KENNEA      | 8          | FRB 8                | 2           | Y   | 0          | 0           |
1720030 | KENNEA      | 9          | FRB 9                | 2           | Y   | 0          | 0           |
1720030 | KENNEA      | 10         | FRB 10               | 2           | Y   | 0          | 0           |
1720038 | GRUPE       | 1          | ESO 242-G8           | 1           | N   | 6.25083    | -45.49278   |
1720038 | GRUPE       | 2          | TON S 180            | 1           | N   | 14.33417   | -22.3825    |
1720038 | GRUPE       | 3          | QSO 0056-36          | 1           | N   | 14.65583   | -36.10139   |
1720038 | GRUPE       | 4          | RX J0100-5113        | 1           | N   | 15.11292   | -51.23167   |
1720038 | GRUPE       | 5          | RX J0105.6-1416      | 1           | N   | 16.41167   | -14.27056   |
1720038 | GRUPE       | 6          | RX J0117-3826        | 1           | N   | 19.3775    | -38.44167   |
1720038 | GRUPE       | 7          | MS 0117-28           | 1           | N   | 19.89875   | -28.35889   |
1720038 | GRUPE       | 8          | RX J0128.1-1848      | 1           | N   | 22.02792   | -18.80861   |
1720038 | GRUPE       | 9          | IRAS F01267-217      | 1           | N   | 22.29458   | -21.69917   |
1720038 | GRUPE       | 10         | RX J0134.2-4258      | 1           | N   | 23.57042   | -42.97417   |
1720038 | GRUPE       | 11         | RX J0136.9-3510      | 1           | N   | 24.22667   | -35.16444   |
1720038 | GRUPE       | 12         | RX J0148.3-2758      | 1           | N   | 27.09292   | -27.97389   |
1720038 | GRUPE       | 13         | RX J0152.4-2319      | 1           | N   | 28.11292   | -23.33167   |
1720038 | GRUPE       | 14         | MKN 1044             | 1           | N   | 37.52292   | -8.99806    |
1720038 | GRUPE       | 15         | MKN 1048             | 1           | N   | 38.6575    | -8.78778    |
1720038 | GRUPE       | 16         | RX J0311.3-2046      | 1           | N   | 47.82833   | -20.77194   |
1720038 | GRUPE       | 17         | RX J0319.8-2627      | 1           | N   | 49.95292   | -26.45333   |
1720038 | GRUPE       | 18         | RX J0323.2-4931      | 1           | N   | 50.81583   | -49.51972   |
1720038 | GRUPE       | 19         | ESO 301-G13          | 1           | N   | 51.26042   | -41.905     |
1720038 | GRUPE       | 20         | VCV 0331-37          | 1           | N   | 53.4175    | -37.11528   |
1720038 | GRUPE       | 21         | RX J0349.1-4711      | 1           | N   | 57.28208   | -47.18444   |
1720038 | GRUPE       | 22         | FAIRALL 1116         | 1           | N   | 57.92375   | -40.46667   |
1720038 | GRUPE       | 23         | FAIRALL 1119         | 1           | N   | 61.25708   | -37.1875    |
1720038 | GRUPE       | 24         | RX J0412.7-4712      | 1           | N   | 63.17292   | -47.21278   |
1720038 | GRUPE       | 25         | 1H 0419-577          | 1           | N   | 66.50292   | -57.20056   |
1720038 | GRUPE       | 26         | FAIRALL 303          | 1           | N   | 67.66667   | -53.61556   |
1720038 | GRUPE       | 27         | RX J0437.4-4711      | 1           | N   | 69.3675    | -47.19167   |
1720038 | GRUPE       | 28         | RX J0439.6-5311      | 1           | N   | 69.91125   | -53.19194   |
1720038 | GRUPE       | 29         | 1H 0439-272          | 1           | N   | 70.34375   | -27.13889   |
1720038 | GRUPE       | 30         | 1 ES 0614-584        | 1           | N   | 93.95667   | -58.435     |
1720038 | GRUPE       | 31         | RX J0859.0+4846      | 1           | N   | 134.76208  | 48.76917    |
1720038 | GRUPE       | 32         | RX J0902.5-0700      | 1           | N   | 135.64     | -7.00111    |
1720038 | GRUPE       | 33         | MKN 110              | 1           | N   | 141.30417  | 52.28667    |
1720038 | GRUPE       | 34         | PG 0953+414          | 1           | N   | 149.21833  | 41.25611    |
1720038 | GRUPE       | 35         | RX J1005.7+4332      | 1           | N   | 151.42458  | 43.54472    |
1720038 | GRUPE       | 36         | RX J1007.1+2203      | 1           | N   | 151.7925   | 22.05056    |
1720038 | GRUPE       | 37         | CBS 126              | 1           | N   | 153.2625   | 35.85667    |
1720038 | GRUPE       | 38         | HS 1019+37           | 1           | N   | 154.75208  | 37.87806    |
1720038 | GRUPE       | 39         | MKN 141              | 1           | N   | 154.8025   | 63.9675     |
1720038 | GRUPE       | 40         | MKN 142              | 1           | N   | 156.38042  | 51.67639    |
1720038 | GRUPE       | 41         | RX J1034.6+3938      | 1           | N   | 158.66083  | 39.64111    |
1720038 | GRUPE       | 42         | RX J1117.1+6522      | 1           | N   | 169.29208  | 65.36861    |
1720038 | GRUPE       | 43         | PG 1115+407          | 1           | N   | 169.62667  | 40.43194    |
1720038 | GRUPE       | 44         | TON 1388             | 1           | N   | 169.78625  | 21.32167    |
1720038 | GRUPE       | 45         | EXO 1128+69          | 1           | N   | 172.77     | 68.86472    |
1720038 | GRUPE       | 46         | 2B 1128+31           | 1           | N   | 172.78958  | 31.235      |
1720038 | GRUPE       | 47         | SBS 1136+579         | 1           | N   | 174.70667  | 57.71222    |
1720038 | GRUPE       | 48         | Z 1136+3412          | 1           | N   | 174.80792  | 33.93083    |
1720038 | GRUPE       | 49         | WAS 26               | 1           | N   | 175.3175   | 21.93917    |
1720038 | GRUPE       | 50         | CASG 855             | 1           | N   | 176.12458  | 36.88583    |
1720038 | GRUPE       | 51         | MKN 1310             | 1           | N   | 180.31     | -3.67806    |
1720038 | GRUPE       | 52         | NGC 4051             | 1           | N   | 180.78958  | 44.53056    |
1720038 | GRUPE       | 53         | GQ COMAE             | 1           | N   | 181.17542  | 27.90333    |
1720038 | GRUPE       | 54         | RX J1209.8+3217      | 1           | N   | 182.43833  | 32.28389    |
1720038 | GRUPE       | 55         | PG 1211+143          | 1           | N   | 183.57375  | 14.05361    |
1720038 | GRUPE       | 56         | MKN 766              | 1           | N   | 184.61083  | 29.81278    |
1720038 | GRUPE       | 57         | 3C 273               | 1           | N   | 187.27792  | 2.0525      |
1720038 | GRUPE       | 58         | RX J1231.6+7044      | 1           | N   | 187.9025   | 70.73722    |
1720038 | GRUPE       | 59         | MKN 771              | 1           | N   | 188.015    | 20.15833    |
1720038 | GRUPE       | 60         | TON 83               | 1           | N   | 188.42375  | 31.0175     |
1720038 | GRUPE       | 61         | MCG+08-23-067        | 1           | N   | 189.21333  | 45.65139    |
1720038 | GRUPE       | 62         | NGC 4593             | 1           | N   | 189.91417  | -5.34417    |
1720038 | GRUPE       | 63         | IRAS F12397+3333     | 1           | N   | 190.54417  | 33.28417    |
1720038 | GRUPE       | 64         | PG 1244+026          | 1           | N   | 191.64667  | 2.36917     |
1720038 | GRUPE       | 65         | RX J1304.2+0205      | 1           | N   | 196.07083  | 2.09361     |
1720038 | GRUPE       | 66         | PG 1307+085          | 1           | N   | 197.44583  | 8.33        |
1720038 | GRUPE       | 67         | RX J1314.3+3429      | 1           | N   | 198.59458  | 34.49417    |
1720038 | GRUPE       | 68         | RX J1319.9+5235      | 1           | N   | 199.98792  | 52.5925     |
1720038 | GRUPE       | 69         | PG 1322+659          | 1           | N   | 200.95625  | 65.69667    |
1720038 | GRUPE       | 72         | RX J1355.2+5612      | 1           | N   | 208.81917  | 56.2125     |
1720038 | GRUPE       | 73         | PG 1402+261          | 1           | N   | 211.3175   | 25.92611    |
1720038 | GRUPE       | 74         | RX J1413.6+7029      | 1           | N   | 213.40292  | 70.49722    |
1720038 | GRUPE       | 75         | NGC 5548             | 1           | N   | 214.49583  | 25.13667    |
1720038 | GRUPE       | 76         | QSO 1421-0013        | 1           | N   | 216.01583  | -0.44944    |
1720038 | GRUPE       | 77         | MKN 813              | 1           | N   | 216.85417  | 19.83139    |
1720038 | GRUPE       | 78         | MKN 684              | 1           | N   | 217.76708  | 28.28722    |
1720038 | GRUPE       | 79         | MKN 478              | 1           | N   | 220.53125  | 35.43972    |
1720038 | GRUPE       | 80         | PG 1448+273          | 1           | N   | 222.78667  | 27.1575     |
1720038 | GRUPE       | 81         | MKN 841              | 1           | N   | 226.005    | 10.43778    |
1720038 | GRUPE       | 82         | SBS 1527+564         | 1           | N   | 232.28125  | 56.26861    |
1720038 | GRUPE       | 83         | MKN 493              | 1           | N   | 239.79042  | 35.03       |
1720038 | GRUPE       | 84         | MKN 876              | 1           | N   | 243.48833  | 65.71972    |
1720038 | GRUPE       | 85         | RX J1618.1+3619      | 1           | N   | 244.53917  | 36.33278    |
1720038 | GRUPE       | 86         | KUG 1618+40          | 1           | N   | 244.96375  | 40.98       |
1720038 | GRUPE       | 87         | PG 1626+554          | 1           | N   | 246.98375  | 55.37556    |
1720038 | GRUPE       | 88         | EXO 1627+4014        | 1           | N   | 247.25542  | 40.13333    |
1720038 | GRUPE       | 89         | RX J1702.5+3247      | 1           | N   | 255.62958  | 32.78889    |
1720038 | GRUPE       | 90         | II ZW 136            | 1           | N   | 323.11625  | 10.13889    |
1720038 | GRUPE       | 91         | RX J2146.6-3051      | 1           | N   | 326.65     | -30.8613    |
1720038 | GRUPE       | 92         | ESO 404-G029         | 1           | N   | 331.9375   | -32.5836    |
1720038 | GRUPE       | 93         | NGC 7214             | 1           | N   | 332.27917  | -27.81      |
1720038 | GRUPE       | 94         | RX J2216.8-4451      | 1           | N   | 334.22167  | -44.8658    |
1720038 | GRUPE       | 95         | RX J2217.9-5941      | 1           | N   | 334.48583  | -59.6916    |
1720038 | GRUPE       | 96         | PKS 2227-399         | 1           | N   | 337.66792  | -39.7144    |
1720038 | GRUPE       | 97         | RX J2242.6-3845      | 1           | N   | 340.65708  | -38.7544    |
1720038 | GRUPE       | 98         | RX J2245.2-4652      | 1           | N   | 341.33458  | -46.87      |
1720038 | GRUPE       | 99         | MS 2254-36           | 1           | N   | 344.4125   | -36.9352    |
1720038 | GRUPE       | 100        | RX J2258.7-2609      | 1           | N   | 344.68917  | -26.1538    |
1720038 | GRUPE       | 101        | RX J2301.6-5913      | 1           | N   | 345.40083  | -59.2222    |
1720038 | GRUPE       | 102        | RX J2301.8-5508      | 1           | N   | 345.46667  | -55.1419    |
1720038 | GRUPE       | 103        | RX J2304.6-3501      | 1           | N   | 346.15542  | -35.0202    |
1720038 | GRUPE       | 104        | RX J2312.5-3404      | 1           | N   | 348.145    | -34.0722    |
1720038 | GRUPE       | 105        | RX J2317.8-4422      | 1           | N   | 349.45792  | -44.3744    |
1720038 | GRUPE       | 106        | RX J2325.2-3236      | 1           | N   | 351.29917  | -32.6097    |
1720038 | GRUPE       | 107        | IRAS F23226-3843     | 1           | N   | 351.35083  | -38.4469    |
1720038 | GRUPE       | 108        | MS 23409-1511        | 1           | N   | 355.86917  | -14.925     |
1720038 | GRUPE       | 109        | RX J2349.4-3126      | 1           | N   | 357.35042  | -31.4341    |
1720038 | GRUPE       | 110        | AM 2354-304          | 1           | N   | 359.36667  | -30.4611    |
1720039 | GRONWALL    | 1          | CDF-N                | 100         | N   | 189.20042  | 62.23139    |
1720039 | GRONWALL    | 2          | CDF-N                | 100         | N   | 189.20042  | 62.23139    |
1720039 | GRONWALL    | 3          | CDF-N                | 100         | N   | 189.20042  | 62.23139    |
1720039 | GRONWALL    | 4          | CDF-N                | 100         | N   | 189.20042  | 62.23139    |
1720040 | KRUMPE      | 1          | AGN IGNITION 1       | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 2          | AGN IGNITION 2       | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 3          | AGN IGNITION 3       | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 4          | AGN IGNITION 4       | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 5          | AGN IGNITION 5       | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 6          | AGN IGNITION 6       | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 7          | AGN IGNITION 7       | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 8          | AGN IGNITION 8       | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 9          | AGN IGNITION 9       | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 10         | AGN IGNITION 10      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 11         | AGN IGNITION 11      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 12         | AGN IGNITION 12      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 13         | AGN IGNITION 13      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 14         | AGN IGNITION 14      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 15         | AGN IGNITION 15      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 16         | AGN IGNITION 16      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 17         | AGN IGNITION 17      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 18         | AGN IGNITION 18      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 19         | AGN IGNITION 19      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 20         | AGN IGNITION 20      | 3           | Y   | 0          | 0           |
1720040 | KRUMPE      | 21         | AGN SHUT-DOWN 1      | 6           | Y   | 0          | 0           |
1720040 | KRUMPE      | 22         | AGN SHUT-DOWN 2      | 6           | Y   | 0          | 0           |
1720040 | KRUMPE      | 23         | AGN SHUT-DOWN 3      | 6           | Y   | 0          | 0           |
1720040 | KRUMPE      | 24         | AGN SHUT-DOWN 4      | 6           | Y   | 0          | 0           |
1720040 | KRUMPE      | 25         | AGN SHUT-DOWN 5      | 6           | Y   | 0          | 0           |
1720041 | FANG        | 1          | CYGNUSCOCOON1        | 10          | N   | 309.14213  | 42.38053    |
1720041 | FANG        | 2          | CYGNUSCOCOON2        | 10          | N   | 307.55762  | 41.89983    |
1720041 | FANG        | 3          | CYGNUSCOCOON3        | 10          | N   | 307.15892  | 41.3055     |
1720041 | FANG        | 4          | CYGNUSCOCOON4        | 10          | N   | 308.69088  | 38.72442    |
1720041 | FANG        | 5          | CYGNUSCOCOON5        | 10          | N   | 307.07304  | 39.71175    |
1720041 | FANG        | 6          | CYGNUSCOCOON6        | 10          | N   | 305.882    | 42.032      |
1720041 | FANG        | 7          | CYGNUSCOCOON7        | 10          | N   | 306.93538  | 43.89167    |
1720041 | FANG        | 8          | CYGNUSCOCOON8        | 10          | N   | 302.79379  | 40.87192    |
1720041 | FANG        | 9          | CYGNUSCOCOON9        | 10          | N   | 307.08675  | 38.05258    |
1720041 | FANG        | 10         | CYGNUSCOCOON10       | 10          | N   | 310.66246  | 41.34619    |
1720044 | LIU         | 1          | PG 1302-102          | 300         | N   | 196.38754  | -10.55539   |
1720061 | MCHARDY     | 1          | MCG+8-11-11          | 180         | N   | 88.72333   | 46.43933    |
1720065 | CHERNYAKOVA | 1          | PSR B1259-63         | 80          | N   | 195.699    | -63.836     |
1720066 | HOMAN       | 1          | X-RAY TRANSIENT      | 40          | Y   | 0          | 0           |
1720067 | WALTON      | 1          | NGC5907 ULX1         | 104         | N   | 228.99571  | 56.30303    |
1720084 | CACKETT     | 1          | MRK 817              | 320         | N   | 219.092    | 58.79428    |
1720090 | DARNLEY     | 1          | M31N 2008-12A        | 84          | Y   | 11.37037   | 41.90283    |
1720095 | AJELLO      | 1          | 3FHL J1127.8+3615    | 4           | N   | 171.96875  | 36.25528    |
1720095 | AJELLO      | 2          | 3FHL J0121.8+3808    | 4           | N   | 20.4565    | 38.134      |
1720095 | AJELLO      | 3          | 3FHL J0233.0+3742    | 4           | N   | 38.2625    | 37.71561    |
1720095 | AJELLO      | 4          | 3FHL J0243.3+1915    | 4           | N   | 40.84871   | 19.26281    |
1720095 | AJELLO      | 5          | 3FHL J0402.9+6433    | 4           | N   | 60.733     | 64.55639    |
1720095 | AJELLO      | 6          | 3FHL J0459.3+1921    | 4           | N   | 74.84679   | 19.36       |
1720095 | AJELLO      | 7          | 3FHL J0500.6+1903    | 4           | N   | 75.17042   | 19.06589    |
1720095 | AJELLO      | 8          | 3FHL J0501.0+2425    | 4           | N   | 75.25721   | 24.4235     |
1720095 | AJELLO      | 9          | 3FHL J0550.9+5657    | 4           | N   | 87.73858   | 56.95231    |
1720095 | AJELLO      | 10         | 3FHL J0753.9+0452    | 4           | N   | 118.489    | 4.88206     |
1720095 | AJELLO      | 11         | 3FHL J0901.5+6712    | 4           | N   | 135.375    | 67.21289    |
1720095 | AJELLO      | 12         | 3FHL J0950.6+6357    | 4           | N   | 147.664    | 63.96589    |
1720095 | AJELLO      | 13         | 3FHL J1421.5-1654    | 4           | N   | 215.391    | -16.91289   |
1720095 | AJELLO      | 14         | 3FHL J1440.2-2343    | 4           | N   | 220.057    | -23.723     |
1720095 | AJELLO      | 15         | 3FHL J1528.4-6730    | 4           | N   | 232.115    | -67.50881   |
1720095 | AJELLO      | 16         | 3FHL J1602.8-1928    | 4           | N   | 240.722    | -19.4695    |
1720095 | AJELLO      | 17         | 3FHL J1726.2-1710    | 4           | N   | 261.57     | -17.16831   |
1720095 | AJELLO      | 18         | 3FHL J1754.2-4334    | 4           | N   | 268.56     | -43.56881   |
1720095 | AJELLO      | 19         | 3FHL J1849.3-6448    | 4           | N   | 282.45517  | -64.73922   |
1720095 | AJELLO      | 20         | 3FHL J2245.5-1734    | 4           | N   | 341.383    | -17.5705    |
1720097 | YOUNES      | 1          | SGR 0755-2933        | 52          | N   | 118.927    | -29.56367   |
1720100 | TORRES-ALBA | 1          | MRK 477              | 50          | N   | 220.15875  | 53.50442    |
1720105 | CORSI       | 1          | ZTFSN1               | 15          | Y   | 0          | 0           |
1720105 | CORSI       | 2          | ZTFSN2               | 15          | Y   | 0          | 0           |
1720105 | CORSI       | 3          | ZTFSN3               | 15          | Y   | 0          | 0           |
1720111 | JENCSON     | 1          | DLT_1                | 36          | Y   | 0          | 0           |
1720111 | JENCSON     | 2          | DLT_2                | 36          | Y   | 0          | 0           |
1720111 | JENCSON     | 3          | DLT_3                | 36          | Y   | 0          | 0           |
1720111 | JENCSON     | 4          | DLT_4                | 36          | Y   | 0          | 0           |
1720111 | JENCSON     | 5          | DLT_5                | 36          | Y   | 0          | 0           |
1720112 | RAJAGOPAL   | 1          | 3FGL J0028.6+7507    | 2           | N   | 7.05442    | 75.10361    |
1720112 | RAJAGOPAL   | 2          | 3FGL J0039.1+4330    | 2           | N   | 9.78296    | 43.50431    |
1720112 | RAJAGOPAL   | 3          | 3FGL J0055.2-1213    | 2           | N   | 13.79908   | -12.29919   |
1720112 | RAJAGOPAL   | 4          | 3FGL J0116.2-2744    | 2           | N   | 18.98167   | -27.74083   |
1720112 | RAJAGOPAL   | 5          | 3FGL J0121.7+5154    | 2           | N   | 20.61433   | 51.97864    |
1720112 | RAJAGOPAL   | 6          | 3FGL J0139.9+8735    | 2           | N   | 24.80583   | 87.63194    |
1720112 | RAJAGOPAL   | 7          | 3FGL J0150.5-5447    | 2           | N   | 27.68467   | -54.83469   |
1720112 | RAJAGOPAL   | 8          | 3FGL J0156.9-4742    | 2           | N   | 29.19179   | -47.73817   |
1720112 | RAJAGOPAL   | 9          | 3FGL J0211.2-0649    | 2           | N   | 32.82042   | -6.73861    |
1720112 | RAJAGOPAL   | 10         | 3FGL J0213.1-2720    | 2           | N   | 33.2305    | -27.305     |
1720112 | RAJAGOPAL   | 11         | 3FGL J0219.0+2440    | 2           | N   | 34.75171   | 24.75572    |
1720112 | RAJAGOPAL   | 12         | 3FGL J0228.7-3106    | 2           | N   | 36.9285    | -30.99986   |
1720112 | RAJAGOPAL   | 13         | 3FGL J0232.9+2606    | 2           | N   | 38.23483   | 26.16194    |
1720112 | RAJAGOPAL   | 14         | 3FGL J0244.4-8224    | 2           | N   | 42.78846   | -82.44144   |
1720112 | RAJAGOPAL   | 15         | 3FGL J0255.8+0532    | 2           | N   | 43.95629   | 5.56528     |
1720112 | RAJAGOPAL   | 16         | 3FGL J0301.8-2721    | 2           | N   | 45.49171   | -27.46525   |
1720112 | RAJAGOPAL   | 17         | 3FGL J1032.7+3735    | 2           | N   | 158.16967  | 37.64078    |
1720112 | RAJAGOPAL   | 18         | 3FGL J1117.9+5355    | 2           | N   | 169.4885   | 53.93189    |
1720112 | RAJAGOPAL   | 19         | 3FGL J1809.4+2040    | 2           | N   | 272.35604  | 20.69192    |
1720112 | RAJAGOPAL   | 20         | 3FGL J1813.6+0614    | 2           | N   | 273.38921  | 6.26167     |
1720117 | HUNG        | 1          | TDE1                 | 62          | Y   | 0          | 0           |
1720118 | HERVET      | 1          | MRK 421              | 147         | N   | 166.11379  | 38.20883    |
1720122 | LOPEZ NAVAS | 1          | CL                   | 130         | Y   | 0          | 0           |
1720126 | DONAHUE     | 1          | 1H 0323+342          | 6.4         | N   | 51.1715    | 34.17942    |
1720126 | DONAHUE     | 2          | 1H1934-063           | 2.1         | N   | 294.38754  | -6.218      |
1720126 | DONAHUE     | 3          | 3C120                | 1.1         | N   | 68.29625   | 5.35433     |
1720126 | DONAHUE     | 4          | 3C382                | 1.5         | N   | 278.76412  | 32.69633    |
1720126 | DONAHUE     | 5          | 3C390.3              | 1.35        | N   | 280.53746  | 79.77142    |
1720126 | DONAHUE     | 6          | ARK 120              | 1.33        | N   | 79.04758   | -0.14983    |
1720126 | DONAHUE     | 7          | ARK 564              | 3           | N   | 340.66392  | 29.72536    |
1720126 | DONAHUE     | 8          | MCG-6-30-15          | 1           | N   | 203.97379  | -34.29553   |
1720126 | DONAHUE     | 9          | MRK 1018             | 5.5         | N   | 31.56663   | -0.29144    |
1720126 | DONAHUE     | 10         | MRK 110              | 1.75        | N   | 141.30362  | 52.28625    |
1720126 | DONAHUE     | 11         | MRK 279              | 2.1         | N   | 208.26438  | 69.30822    |
1720126 | DONAHUE     | 12         | MRK 335              | 9.5         | N   | 1.58133    | 20.20292    |
1720126 | DONAHUE     | 13         | MRK 509              | 1.05        | N   | 311.04058  | -10.72347   |
1720126 | DONAHUE     | 14         | MRK 590              | 7.5         | N   | 33.63983   | -0.76669    |
1720126 | DONAHUE     | 15         | MRK 79               | 2.7         | N   | 115.63667  | 49.80967    |
1720126 | DONAHUE     | 16         | MRK 841              | 3.3         | N   | 226.005    | 10.43783    |
1720126 | DONAHUE     | 17         | NGC 1365             | 3.9         | N   | 53.40154   | -36.14042   |
1720126 | DONAHUE     | 18         | NGC 3783             | 1.7         | N   | 174.75733  | -37.73867   |
1720126 | DONAHUE     | 19         | NGC 4051             | 2.4         | N   | 180.79004  | 44.53133    |
1720126 | DONAHUE     | 20         | NGC 4151             | 1           | N   | 182.63575  | 39.40572    |
1720126 | DONAHUE     | 21         | NGC 4748             | 5.8         | N   | 193.05192  | -13.41472   |
1720126 | DONAHUE     | 22         | NGC 7469             | 2           | N   | 345.81508  | 8.874       |
1720126 | DONAHUE     | 23         | PG 0804+761          | 7.9         | N   | 122.74417  | 76.04514    |
1720126 | DONAHUE     | 24         | PG 1426+015          | 6.1         | N   | 217.27746  | 1.28514     |
1720126 | DONAHUE     | 25         | RBS1124              | 8           | N   | 187.90183  | 70.73725    |
1720126 | DONAHUE     | 26         | UGC 6728             | 7.5         | N   | 176.31675  | 79.6815     |
1720126 | DONAHUE     | 27         | PG 0844+349          | 10.3        | N   | 131.92692  | 34.75122    |
1720128 | HERVET      | 1          | MRK 421              | 88          | Y   | 166.11375  | 38.20883    |
1720132 | HOMAN       | 1          | NS TRANSIENT         | 48          | Y   | 0          | 0           |
1720137 | MARGUTTI    | 1          | FBOT                 | 90          | Y   | 0          | 0           |
1720139 | AUCHETTL    | 1          | ASASSN-14LI          | 6           | N   | 192.06333  | 17.774      |
1720139 | AUCHETTL    | 2          | ASASSN-15OI          | 7.5         | N   | 309.78825  | -30.75558   |
1720139 | AUCHETTL    | 3          | IPTF16FNL            | 9           | N   | 7.48754    | 32.89367    |
1720139 | AUCHETTL    | 4          | ASASSN-14AE          | 9           | N   | 167.16717  | 34.09783    |
1720139 | AUCHETTL    | 5          | AT2018DYB            | 12.5        | N   | 242.74487  | -60.92308   |
1720139 | AUCHETTL    | 6          | ASASSN-19BT          | 10          | N   | 105.04808  | -66.04003   |
1720139 | AUCHETTL    | 7          | ASASSN-19DJ          | 10          | N   | 123.32058  | 22.64833    |
1720139 | AUCHETTL    | 8          | AT2019QIZ            | 10          | N   | 71.65783   | -10.22636   |
1720141 | MILLER      | 1          | SN IA FLASH TOO-1    | 36          | Y   | 0          | 0           |
1720141 | MILLER      | 2          | SN IA FLASH TOO-2    | 36          | Y   | 0          | 0           |
1720141 | MILLER      | 3          | SN IA TOO-1          | 8           | Y   | 0          | 0           |
1720141 | MILLER      | 4          | SN IA TOO-2          | 8           | Y   | 0          | 0           |
1720141 | MILLER      | 5          | SN IA TOO-3          | 8           | Y   | 0          | 0           |
1720141 | MILLER      | 6          | SN IA TOO-4          | 8           | Y   | 0          | 0           |
1720141 | MILLER      | 7          | SN IA TOO-5          | 8           | Y   | 0          | 0           |
1720141 | MILLER      | 8          | SN IA TOO-6          | 8           | Y   | 0          | 0           |
1720141 | MILLER      | 9          | SN TOO FP-1          | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 10         | SN TOO FP-2          | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 11         | SN TOO FP-3          | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 12         | SN TOO FP-4          | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 13         | SN TOO FP-5          | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 14         | SN TOO FP-6          | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 15         | SN TOO FP-7          | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 16         | SN TOO FP-8          | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 17         | SN TOO FP-9          | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 18         | SN TOO FP-10         | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 19         | SN TOO FP-11         | 4           | Y   | 0          | 0           |
1720141 | MILLER      | 20         | SN TOO FP-12         | 4           | Y   | 0          | 0           |
1720147 | PASHAM      | 1          | 2MASS 02314715-10201 | 90          | N   | 37.94721   | -10.33639   |
1720150 | MARSCHER    | 1          | MKN421               | 4           | N   | 166.11379  | 38.20883    |
1720150 | MARSCHER    | 2          | MKN421               | 27          | N   | 166.11379  | 38.20883    |
1720150 | MARSCHER    | 3          | MKN501               | 4           | N   | 253.46758  | 39.76017    |
1720150 | MARSCHER    | 4          | MKN501               | 27          | N   | 253.46758  | 39.76017    |
1720150 | MARSCHER    | 5          | CENA                 | 4           | N   | 201.36508  | -44.02581   |
1720150 | MARSCHER    | 6          | CENA                 | 9           | N   | 201.36508  | -44.02581   |
1720150 | MARSCHER    | 7          | 3C454.3              | 4           | N   | 343.49062  | 16.14822    |
1720150 | MARSCHER    | 8          | 3C454.3              | 18          | N   | 343.49062  | 16.14822    |
1720150 | MARSCHER    | 9          | 3C279                | 4           | N   | 194.04654  | -5.78931    |
1720150 | MARSCHER    | 10         | 3C279                | 18          | N   | 194.04654  | -5.78931    |
1720150 | MARSCHER    | 11         | 1ES1959+65           | 4           | N   | 299.99942  | 65.1485     |
1720150 | MARSCHER    | 12         | 1ES1959+65           | 18          | N   | 299.99942  | 65.1485     |
1720150 | MARSCHER    | 13         | BLLAC                | 6           | N   | 339.68038  | 42.27778    |
1720150 | MARSCHER    | 14         | BLLAC                | 18          | N   | 339.68038  | 42.27778    |
1720150 | MARSCHER    | 15         | J0211+1051           | 6           | N   | 32.80492   | 10.85967    |
1720150 | MARSCHER    | 16         | 0716+714             | 6           | N   | 110.47271  | 71.34339    |
1720150 | MARSCHER    | 17         | 1ES0229+20           | 6           | N   | 38.20258   | 20.28819    |
1720150 | MARSCHER    | 18         | PKS2155-30           | 6           | N   | 329.71696  | -30.22558   |
1720152 | SAKAMOTO    | 1          | MAXI GRB             | 2.8         | Y   | 0          | 0           |
1720152 | SAKAMOTO    | 2          | MAXI GRB             | 2.8         | Y   | 0          | 0           |
1720152 | SAKAMOTO    | 3          | MAXI GRB             | 2.8         | Y   | 0          | 0           |
1720152 | SAKAMOTO    | 4          | MAXI GRB             | 2.8         | Y   | 0          | 0           |
1720156 | TERRERAN    | 1          | SLSN1                | 110         | Y   | 0          | 0           |
1720156 | TERRERAN    | 2          | SLSN2                | 110         | Y   | 0          | 0           |
1720157 | CHORNOCK    | 1          | INTERACTINGSN1       | 49          | Y   | 0          | 0           |
1720157 | CHORNOCK    | 2          | INTERACTINGSN2       | 49          | Y   | 0          | 0           |
1720161 | WARGELIN    | 1          | PROXIMA CEN          | 36          | N   | 217.37917  | -62.67483   |
1720170 | MCCARRIE    | 1          | GRB090515            | 40          | N   | 164.15129  | 14.44181    |
1720170 | MCCARRIE    | 2          | GRB070809            | 40          | N   | 203.76971  | -22.14167   |
1720173 | TRUMP       | 1          | 1H0419-577           | 1           | N   | 66.503     | -57.20028   |
1720173 | TRUMP       | 2          | 1H0707-495           | 1.6         | N   | 107.17292  | -49.55192   |
1720173 | TRUMP       | 3          | ARK 120              | 1           | N   | 79.04758   | -0.14983    |
1720173 | TRUMP       | 4          | ARK 564              | 1           | N   | 340.66396  | 29.72536    |
1720173 | TRUMP       | 5          | ESO 362-G18          | 1           | N   | 79.89917   | -32.65758   |
1720173 | TRUMP       | 6          | IRAS 13224-3809      | 2.1         | N   | 201.33075  | -38.41464   |
1720173 | TRUMP       | 7          | MCG-6-30-15          | 2.1         | N   | 203.97379  | -34.29553   |
1720173 | TRUMP       | 8          | MRK 359              | 1           | N   | 21.88562   | 19.17883    |
1720173 | TRUMP       | 9          | MRK 1018             | 1           | N   | 31.56663   | -0.29144    |
1720173 | TRUMP       | 10         | MRK 79               | 1           | N   | 115.63667  | 49.80964    |
1720173 | TRUMP       | 11         | MRK 841              | 1           | N   | 226.005    | 10.43783    |
1720173 | TRUMP       | 12         | NGC 1365             | 1           | N   | 53.40154   | -36.14039   |
1720173 | TRUMP       | 13         | NGC 4051             | 1           | N   | 180.79004  | 44.53133    |
1720173 | TRUMP       | 14         | NGC 7469             | 1           | N   | 345.81508  | 8.874       |
1720173 | TRUMP       | 15         | SWIFT J2127+5654     | 1           | N   | 321.93729  | 56.94436    |
1720173 | TRUMP       | 16         | TONS180              | 1.05        | N   | 14.33308   | -22.38308   |
1720173 | TRUMP       | 17         | H1821+643            | 1           | N   | 275.48879  | 64.34344    |
1720173 | TRUMP       | 18         | NGC 3783             | 1           | N   | 174.75733  | -37.73867   |
1720180 | SANTANDER   | 1          | NEUTRINO TARGET1     | 12          | Y   | 0          | 0           |
1720180 | SANTANDER   | 2          | NEUTRINO TARGET2     | 12          | Y   | 0          | 0           |
1720183 | BODEWITS    | 1          | C/2017 K2            | 67.2        | N   | 0          | 0           |


## Proposal Abstracts

1720002 / BOGDANOV / COLUMBIA UNIVERSITY

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

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

1720004 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY

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

We propose 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.

1720006 / GAIDOS / UNIVERSITY OF HAWAII (MANOA)

"X-RAYING THE INNER DISK OF A 'DIPPER' STAR WITH SWIFT"

We propose simultaneous UV/X-ray/optical monitoring of the 4-10 Myr-old T Tauri star EP Chamaeleontis with Swift, TESS, and ground-based telescopes to better understand the structure and composition of the inner circumstellar disk (<1 AU) where planets are expected to form. EP Cha exhibits pronounced episodic dimming ('dipping') due to circumstellar dust, and our data, obtained both during and outside of dimming events, will constrain dust grain properties, locate the dust relative to sources of UV emission, and measure the relative gas/dust ratio, thereby testing models of dimming events and inner disk structure during a critical, late stage of evolution.

1720020 / MACCARONE / TEXAS TECH UNIVERSITY

"THE SWIFT GALACTIC BULGE MONITORING SURVEY: THIRD 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.

1720030 / KENNEA / THE PENNSYLVANIA STATE UNIVERSITY

"RAPID SWIFT FOLLOW-UP OF FAST RADIO BURSTS"

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

1720038 / GRUPE / MOREHEAD STATE UNIVERSITY

"CATCHING AGN IN EXTREME X-RAY AND UV FLUX STATES"

The idea of this proposal re-observe a sample of 110 X-ray bright AGN previously observed by Swift 1 ks each in order to to identify at least one of these AGN in an extreme X-ray flux state. This will then trigger an ongoing XMM/NuStar/HST ToO program aiming to investigate in detail the X-ray and UV 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.

1720039 / GRONWALL / THE PENNSYLVANIA STATE UNIVERSITY

"DEEP UVOT IMAGING OF GOODS-NORTH"

We propose deep UVOT imaging of GOODS-North (Great Observatories Origins Deep Survey) in the near-UV as well as simultaneous XRT imaging. Deep Swift observations of GOODS-N will allow measurements of galaxy evolution through UV galaxy number counts, galaxy luminosity functions, and the identification and characterization of Lyman break galaxies in the 0.5 < z < 2.0 redshift range. Simultaneous XRT data will provide variability information on critical timescales that are inaccessible with the existing data. This program is complementary to the earlier UVOT observations of the Chandra Deep Field South (CDF-S) in that it will provide improved statistics on galaxy counts and address biases due to cosmic variance.

1720040 / KRUMPE / LEIBNIZ-INSTITUT FUR ASTROPHYSIK POTSDAM (AIP)

"EROSITA FOLLOW-UP OF RARE AGN IGNITIONS AND SHUT-DOWN EVENTS"

eROSITA, launched in mid-2019, is performing multiple all-sky X-ray surveys. Monitoring almost half a million AGN/quasars every six months, eROSITA will identify rare, accretion ignition/shut-down events as they occur. We propose 25 ToOs (20 with 3 ks - ignition event; five with 6 ks - shut-down event). The first results of an approved DDT request for 5 objects showed how beneficial the additional Swift data are to i) explore the X-ray evolution on time scales shorter than six months, ii) decide for the best follow-up strategy using additional triggers on other facilities, and iii) complete the multi-wavelength view with UV coverage. The latter will also be used to constrain the SED and derive accretion disk temperatures.

1720041 / FANG / UNIVERSITY OF WISCONSIN-MADISON

"DIAGNOSE THE GAMMA-RAY EMISSION MECHANISM OF THE CYGNUS COCOON WITH SWIFT-XRT"

The Cygnus Cocoon has been detected by the Fermi-LAT and recently by the HAWC Observatory, making it the first and the only stellar superbubble seen in both GeV and TeV energies. An unsolved question by gamma-ray observations is whether the emission comes from leptons or hadrons. The key to finding the origin of the gamma-rays is to find or exclude the Synchrotron emission by relativistic leptons. We propose to observe the Cygnus Cocoon with Swift-XRT. By sampling the Cocoon with ten pointings, and comparing the on- and off-source X-ray emission levels, the proposed observation will justify whether excess X-ray emission is associated with the gamma-ray emitting regions. This project will connect Swift observations with multi-messenger studies of cosmic accelerators.

1720044 / LIU / UNIVERSITY OF WISCONSIN-MILWAUKEE

"SWIFT REVERBERATION MAPPING OF A SUPERMASSIVE BLACK HOLE BINARY CANDIDATE"

The quasar PG 1302-102 has been proposed as a candidate supermassive black hole binary (SMBHB) at a sub-parsec separation, but its binary hypothesis is still the subject of vigorous debate. Here we propose a novel test of the binary hypothesis of PG 1302-102 which applies the technique of AGN disk reverberation mapping and directly constrains the presence of a "minidisk," which is the accretion disk around one of the binary components and a robust prediction in numerical simulations of accreting SMBHBs.

1720046 / SICILIAN / UNIVERSITY OF MIAMI

"CONSTRAINING THE STERILE NEUTRINO DARK MATTER PARAMETER SPACE WITH ARCHIVAL SWIFT DATA"

The sterile neutrino is a dark matter candidate with decay detectable by X-ray observatories. Recently, a feature at 3.5 keV has been hypothesized as arising from sterile neutrino dark matter. We propose a comprehensive search for the sterile neutrino decay signature in the Milky Way Halo using ~188 Ms of archival Swift XRT data. We will investigate possible faint signals across the continuum, including 3.5 keV, and use non-detections to constrain the parameter space. We will map the line flux or upper-limits across the Halo for comparison to dark matter profiles to consider the dark matter interpretation. A detection would be highly significant, contributing strongly towards an understanding of dark matter. Non-detections would rule out keV sterile neutrino dark matter almost entirely.

1720050 / DURBAK / UNIVERSITY OF MARYLAND (COLLEGE PARK)

"RIMAS: THE RAPID IMAGER AND SPECTROGRAPH; A NEW TOOL FOR HIGH-REDSHIFT GRBS"

RIMAS is a new NIR instrument designed expressly to identify high-redshift gamma-ray bursts (GRBs) from Swift, to be installed on the 4.3m Lowell Discovery Telescope(LDT). RIMAS can operate in and switch rapidly (10s of seconds) between 3 modes: 1)simultaneous 2-band imaging; 2)high-throughput, R~25 NIR spectroscopy; 3)high-resolution (R~4500), cross-dispersed echelle spectroscopy providing simultaneous coverage from 0.9--2.4 micron. Unlike most classically scheduled facilities, RIMAS will be continuously available for rapid-response (dt<3 minutes) ToO observations. By the end of Cycle 17, RIMAS will be routinely obtaining rapid multi-color photometry and NIR spectra of Swift afterglows to measure their redshifts and constrain properties of their host galaxies and the surrounding IGM.

1720061 / MCHARDY / UNIVERSITY OF SOUTHAMPTON

"REVERBERATION MAPPING OF THE HIGH ACCRETION RATE AGN MCG+08-11-11"

Swift reverberation mapping (RM) has greatly improved our understanding of the inner regions of AGN but has highlighted important questions. 1) Disc reprocessing of high energies explains much UV/optical variability but implied disc sizes are too big. 2)There is evidence for a second reprocessor, possibly the broad line region (BLR). 3) The UV to X-ray lags are longer than excpected from disc repro- cessing. Accretion rate (mdot) might be important as it affects inner BLR radius and disc structure. However, with one exception, only low mdot AGN have been studied. A Swift/VLA daily monitoring for 90d of the very X-ray bright AGN MCG+08-11-11 has been already approved. Here we ask to raise Swift sampling to 3 per day in order to perform high quality RM of this AGN together with LCO data.

1720065 / CHERNYAKOVA / DUBLIN CITY UNIVERSITY

"SWIFT OBSERVATIONS OF PSR B1259-63 DURING ITS 2021 PERIASTRON PASSAGE"

This proposal is to use Swift to observe the 2021 periastron passage of PSR B1259-63 within the framework of a large multi-wavelength campaign, where extensive optical (SALT) and radio (ATCA) monitoring has already been approved. Such a campaign will allow us to study the structure of the Be star disk, and the details of the interaction of the pulsar wind and the stellar wind. The periastron in 2021 is the best period for such a campaign since ground-based observations during the next two periastra will be far less feasible.

1720066 / 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. With our program we aim 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 a monitoring campaign for one transient, with daily 2 ks observations for 20 days.

1720067 / WALTON / UNIVERSITY OF CAMBRIDGE

"TESTING THE LENSE-THIRRING MODEL FOR ULX VARIABILITY WITH NGC5907 ULX1"

Following a series of remarkable recent discoveries, it is now clear that some of the ultraluminous X-ray source (ULX) population are actually powered by highly super-Eddington neutron stars. NGC5907 ULX1 is the most extreme of these, exhibiting a remarkable peak luminosity of ~1e41 erg/s, as well as X-ray off-states (where the flux drops by a factor of ~100 or more) and a clear ~78d super-orbital X-ray period when active. Although the source has spent most of the last few years in an off-state, it has now returned to its ULX state and is also showing evidence for having re-established its 78d cycle. This presents a unique opportunity to test the Lense-Thirring interpretation for the super-orbital periods seen in ULX pulsars with continued Swift monitoring.

1720084 / CACKETT / WAYNE STATE UNIVERSITY

"AGN REVERBERATION MAPPING OF GAS FLOWS IN MRK 817 WITH SWIFT AND HUBBLE"

Knowledge of the structure and kinematics of gas around supermassive black holes is vital to understanding accretion and thus AGN feedback. To this end, Mrk 817 will be the subject of a large, multiwavelength reverberation mapping campaign built around an already-approved 198-orbit Hubble Large Program. We propose a Swift Key Project to provide 320 daily observations of Mrk 817. Swift's role is critical, providing high cadence X-ray/UV/optical lightcurves against which to measure lags. Swift enables answering key questions regarding accretion disk size and origin of the continuum emission, while also tracking changes in the spectral energy distribution. This legacy-quality dataset is unlikely to be replicated as inevitable loss of gyros will limit Hubble's future monitoring capabilities.

1720090 / DARNLEY / LIVERPOOL JOHN MOORES 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 11 observed eruptions in 11 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 2020 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.

1720095 / AJELLO / CLEMSON UNIVERSITY

"TOWARDS THE FULL IDENTIFICATION OF THE 3FHL CATALOG"

We propose to use Swift to search for X-ray and optical/UV counterparts of the 20 brightest unassociated objects in the 3FHL catalog. This catalog of sources detected by Fermi/LAT above 10 GeV is the deepest look at the very high-energy sky and will be used by CTA to plan most of the observations. Making it as complete as possible will result in stronger detections and characterizations of the EBL, better understanding of the origin of the IceCube neutrino flux and better planning for CTA. These observations will be coupled to our ongoing optical spectroscopic and photometric campaigns to measure the redshift of the proposed objects rendering this program highly efficient.

1720097 / YOUNES / GEORGE WASHINGTON UNIVERSITY

"SWIFT X-RAY MONITORING OF THE MAGNETAR SGR 0755-2933"

Magnetars are young isolated neutron stars with thermal soft X-ray emission resulting from the decay of their internal magnetic field. SGR 0755-2933 is a magnetar discovered as a bright X-ray source in March 2016 after it emitted a magnetar-like burst. Its X-ray flux decayed steadily in the following months to a level 2 orders of magnitude fainter than at outburst onset. Subsequent XRT observations up to 2020 September, albeit sparse, indicate an unprecedented outbrust rate of >1 per year. Moreover, the source XRT position is coincident with a bright optical counterpart. Here, we propose a bi-weekly monitoring campaign of SGR 0755-2933 to establish its yearly variability pattern, allowing for a better understanding of the place of this intriguing source within the larger magnetar family.

1720100 / TORRES-ALBA / CLEMSON UNIVERSITY

"PROBING THE STRUCTURE OF THE AGN TORUS WITH SWIFT"

AGN are assumed to be obscured by a dusty gas torus, originally described as homogeneous. Recent studies show variability in the hydrogen column density of this obscuring material, leading us to believe the torus is patchy rather than uniform. However, the assumption that a patchy torus is responsible for all obscuration in AGN is incompatible with sources without variability, and with those that only show it on yearly timescales. We propose to monitor the bright Sy2 Mrk 477, which shows yearly variability but lacks observations probing timescales of weeks to months, with five 10 ks snapshots with XRT. Detecting variability would allow us to derive a complete picture of the properties of its absorber. Not detecting it would force us to consider more complex scenarios.

1720105 / CORSI / TEXAS TECH UNIVERSITY

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

The rare class of massive-star explosions dubbed broad-lined (BL) Type Ic supernovae (SNe), estimated to constitute only 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). GRBs are the most relativistic explosions arising from a collapsing compact object. What makes some BL-Ic SNe produce a GRB remains a mystery. Two key questions are yet to be answered: (i) Why do only a fraction of BL-Ic SNe have relativistic ejecta powering radio/X-ray afterglows? (ii) Are low-luminosity GRBs beamed? This proposal aims at answering both of these questions via follow-up observations of SNe discovered by the Zwicky Transient Facility (ZTF), using the Neil Gehrels Swift observatory and the Karl G. Jansky VLA.

1720111 / JENCSON / UNIVERSITY OF ARIZONA

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

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

1720112 / RAJAGOPAL / CLEMSON UNIVERSITY

"HUNTING HIGH REDSHIFT BLAZARS WITH SWIFT AND SARA-CT/ORM"

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.

1720117 / HUNG / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)

"EARLY UV AND X-RAY EVOLUTION OF TIDAL DISRUPTION EVENTS IN YSE"

The Young Supernova Experiment (YSE) has begun operating in full swing and is poised to find tidal disruption events (TDEs) before maximum light, granting us the opportunity to track the most crucial, yet currently missing, phase of their evolution. Early sciences of TDEs will advance our understanding in the emission mechanisms acting in these fascinating transients, which are linked to some of the most important astrophysical questions: black hole demographics, disk formation and super-Eddington accretion. We propose to monitor 1 TDE discovered before peak with Swift for a duration of 90 days. These data will put constraints on the early-time TDE energetics, which is critical for breaking the degeneracies in current TDE emission models as we continue to explore the TDE phase space.

1720118 / HERVET / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)

"DAILY MONITORING OF MRK 421 FOR AN UNPRECEDENTED MULTI-WAVELENGTH VARIABILITY STUDY"

Most blazars are studied only when triggered as a target of opportunity (ToO). Unfortunately this strategy gives only sparse information on their standard behavior/regime. Resolving this issue requires a deep change of the usual observation strategy, moving from ToO to long, dense, and simultaneous multi-wavelength observations. Mrk421 is the perfect candidate for such a campaign. It is the only HBL bright enough in Fermi-LAT for daily measured fluxes, and it is already observed daily by VERITAS. Having simultaneous Swift observations will provide unprecedented material to deeply study the nominal behavior of a TeV HBL. It would also bring critical clues addressed to specific issues of Mrk421 such as a possible pattern of repeating flares, or different populations of radiative particles.

1720122 / LOPEZ NAVAS / UNIVERSIDAD DE VALPARAISO

"MULTI WAVELENGTH MONITORING OF A CHANGING-LOOK PHENOMENON"

Recently, a new class of extremely variable AGNs has been discovered: the changing-look (CL) AGN, which show an appearance or disappearance of their BELs. Last year, a CL event followed by a destruction and recreation of the X ray corona was monitored in a time scale of <1 year. This implies CL events can be associated with dramatic and rapid transformations of the innermost regions of AGNs. Here we propose a 200 days multiwavelength monitoring of a ToO CL candidate discovered through their current optical variability and past Sy2 classification. Our observations are needed to track the evolution and simultaneity of the optical/UV emission from the disc and the X ray corona. This effort is crucial to develop the framework by which we can understand the CL nature and infer their properties.

1720126 / DONAHUE / MICHIGAN STATE UNIVERSITY

"A NEW METHOD TO OBTAIN BLACK HOLE SPIN VALUES WITH 27 LOCAL AGN"

Black hole spin is a key property that describes a black hole. Recently, a new method of determining black hole spin was proposed and applied to over 700 sources including supermassive and stellar-mass black holes. We request observations of AGN to test the new method, called the outflow method, to make new spin determinations. The proposed sample has published spin values obtained with the X-ray reflection method. A comparison of spin values obtained independently with the outflow and X-ray reflection methods will indicate the viability of the new method and its range of application. Mass accretion rates of AGN will also be obtained with the data requested here by applying the outflow model and these will be compared with independently determined published values.

1720128 / HERVET / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)

"TOWARD A CONFIRMATION OF MULTIPLE RECOLLIMATION SHOCKS IN THE BL LAC MRK 421"

The origin and location of the non-thermal particle acceleration zone in active galactic nuclei (AGN) jets is one of the major questions still pending for these objects. The current consensus scenario involves a first-order Fermi process of a highly relativistic flow passing through a strong shock close to or in the radio core, revealed by very long baseline interferometry (VLBI). The common observations of multiple stationary VLBI knots in high-frequency-peaked BL Lacs (HBLs) can be interpreted as multiple recollimation shocks accelerating particles along jets. Hence, a unique pattern of the variability should appear after each strong flare from an X-ray bright HBL such as Mrk 421. This should produce observational features that are particularly well suited to the capabilities of Swift.

1720132 / HOMAN / EUREKA SCIENTIFIC INC.

"INVESTIGATING SHALLOW HEATING IN NEUTRON STAR CRUSTS"

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

1720137 / MARGUTTI / NORTHWESTERN UNIVERSITY

"A FOCUSED SWIFT INVESTIGATION OF FAST BLUE OPTICAL TRANSIENTS"

ABSTRACT: Fast and Blue Optical Transients (FBOTs) are a new class of stellar explosions. With extremely rapid time scales of evolution and luminous emission, FBOTs probe the extremes of the explosion parameters and/or stellar progenitor properties, and are hard to reconcile within the traditional supernova models. Alternative scenarios include strong shock interaction with a dense medium, or the presence of a central engine (e.g. BH or magnetar formed by the explosion). Here we propose a focused investigation of the closest FBOTs (d<300 Mpc) with Swift as part of our extensive multi-wavelength monitoring program (radio to X-rays). By densely sampling the UV and X-ray properties of FBOTs with Swift, our overarching goal is to advance our understanding of their intrinsic nature.

1720139 / AUCHETTL / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)

"THE FINAL STAGES OF BRIGHT OPTICAL TDES"

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

1720141 / MILLER / NORTHWESTERN UNIVERSITY

"A SWIFT RESPONSE TO THERMONUCLEAR EXPLOSIONS"

We propose a new program utilizing Swift to obtain ultraviolet (UV) observations of type Ia supernovae (SNe Ia) in the moments after they explode. Deciphering the progenitors of SNe Ia is hindered by the fact that they all have a nearly identical appearance around maximum light (the epoch when they are most easily observed). To answer lingering questions about the progenitor system (including, what is the nature of the binary companion and what is the mass of the exploding white dwarf), we will undertake an ambitious program to automatically identify young SNe and trigger Swift. UV ToO observations are uniquely poised to break observational degeneracies in the optical and advance our understanding of thermonuclear SNe.

1720147 / PASHAM / MASSACHUSETTS INSTITUTE OF TECHNOLOGY

"TRACKING THE LONG-TERM EVOLUTION OF QUASI-PERIODIC ERUPTIONS FROM A NEWLY DISCOVERED EROSITA AGN USING XRT AND UVOT"

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 flows. We request a minimum of 2 sets (3 preferred) of high-cadence XRT and UVOT monitoring observations (15 visits/day for 4 days per set) of QPEs in 2MASS 02314715-1020112 discovered by eROSITA and NICER (quasi-period of 0.8 d). 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 one year, and 2) search for correlations between the X-ray and UV emission. This requires high-cadence X-ray+UV monitoring and currently only Swift can perform such observations.

1720150 / MARSCHER / BOSTON UNIVERSITY

"MONITORING IXPE BLAZAR TARGETS WITH SWIFT"

The investigators propose to observe 10 X-ray bright blazars multiple times with the Swift XRT and UVOT. The selected blazars are planned targets for IXPE X-ray (2-8 keV) linear polarization measurements. The Swift observations will determine which blazars are bright enough to be observed by IXPE and provide X-ray and UVOT continuum spectra. Comparison of the millimeter-wave, optical, and X-ray polarization and measurement of the mm--optical--UV--X-ray continuum spectra of the blazars, will provide data needed to determine the mechanism and location of the X-ray emission, which have yet to be determined conclusively. It will also test models for particle acceleration that produces high-energy emission in relativistic jets.

1720152 / 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" 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 (400 s per tiling) to search for an X-ray afterglow candidate for the MAXI XRFs and LLGRBs. We also request additional follow-up observations when a possible candidate is identified.

1720156 / 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) 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.

1720157 / CHORNOCK / NORTHWESTERN UNIVERSITY

"DETAILED MAPPING OF EXTREME MASS-LOSS FROM EVOLVED MASSIVE STARS WITH SWIFT"

Contrary to expectations from current stellar evolutionary models, recent observations uncovered the ejection of shells of material by massive stars in the years before the supernova explosion, thus revealing our inadequate understanding of the last stages of evolution of massive stars. Here we propose a focused Swift project, with the aim to (i) constrain the mass-loss history of massive stars before explosion, employing multi-wavelength observations of the supernova shock breaking out through a dense medium; and (ii) constrain the efficiency of cosmic-ray acceleration by supernova shocks. This study will open up a new window of investigation on the SN shock-circumstellar medium interaction.

1720161 / WARGELIN / SMITHSONIAN ASTROPHYSICAL OBSERVATORY

"DOES PROXIMA CENTAURI REALLY HAVE A STELLAR CYCLE?"

A few years ago, it was reported that Proxima Cen, a fully convective dM5.5e star, has a solar-like 7-year stellar cycle. This surprising result was based on roughly a decade of optical monitoring data, with some supporting evidence from Swift X-ray and UV observations. Additional observations since that time have yielded puzzling optical data, while strengthening the case for an X-ray cycle. We request twelve 3-ks observations with 8-day spacing to extend long term X-ray/UV study of Proxima in order to better establish the existence and properties of the apparent cycle. Proxima is the only fully convective star practical for such work, and Swift is uniquely well suited for the challenges of monitoring high-energy emission from this flare star.

1720170 / MCCARRIE / POMONA COLLEGE

"SHORT GRBS IN CLUSTERS OF GALAXIES"

The environment of short duration gamma-ray bursts (GRBs) yields fundamental clues about the nature of their progenitors. Here we propose a Swift fill-in program to explore the association between short GRBs and galaxy clusters. The proposed observation will allow us to confirm the proposed association, based on an over-density of optical galaxies, and to better characterize the relationship between short GRBs and galaxy clusters - so far based on a single firm association.

1720171 / MOCKLER / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)

"MOSFIT: CONNECTING MODELS TO TIDAL DISRUPTION EVENT OBSERVATIONS"

Over the next several years, transient surveys will provide more and higher fidelity data of tidal disruption events (TDEs). By modeling TDE light curves one can study: the size of super-massive black holes (SMBHs) in quiescent galaxies, stellar populations in galactic nuclei, and the physics of SMBH accretion under well-defined conditions. This has been done extensively using the publicly available code MOSFiT. However, the library of hydrodynamical simulations that provides the engine in MOSFiT's TDE model relies on outdated models of stellar disruptions. We propose to update the code by incorporating a more realistic library of disruption simulations. This will improve MOSFiT s accuracy, enabling better characterization of the SMBH and the dense stellar clusters that surround them.

1720173 / TRUMP / UNIVERSITY OF CONNECTICUT

"BLACK HOLE SPIN FROM CONTEMPORANEOUS UV-OPTICAL SEDS"

We propose ultraviolet imaging with Swift/UVOT to measure black hole spin for 18 AGN. Our target AGN are selected to have previous Fe Ka spin measurements from X-ray spectroscopy, and we will compare our new spins from Swift with the previous Fe Ka measurements to calibrate the models and methodology for SED fits of black hole spin. Unlike Fe Ka, SED-based spins can be measured for AGN over wide ranges in luminosity and redshift. This proposal represents the first step in developing a new method that enables measurement of black hole spin evolution across cosmic time.

1720180 / SANTANDER / UNIVERSITY OF ALABAMA

"PROBING THE NEUTRINO-BLAZAR CONNECTION 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.

1720183 / BODEWITS / AUBURN UNIVERSITY

"CHARACTERIZING THE DISTANT ACTIVITY EVOLUTION OF COMET C/2017 K2 (PANSTARRS)"

The goal of this project is to investigate the effects of comet activity at large distances from the Sun, where the nucleus is too cold for water to effectively sublimate, and to compare this to sublimation driven comet activity in the inner solar system. For this, we request 48 orbits of Swift/UVOT observations of comet C/2017 K2 (PanSTARRS). This mysterious object has been active at the unprecedented large distance of 25 au while approaching the Sun, where its surface has very low temperatures. Combing its activity levels and brightness with Swift s capabilities provides a unique opportunity to study cometary activity over a broad range of heliocentric distances. This will provide critical information on different mechanisms through which comets evolve and will also allow us to study how