The lists below contain the proposals recommended by the Cycle 12 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 12 proposals for observation: Please note that the ROSES 2015 Appendix D.5 "Swift Guest Investigator Cycle 12" 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/secure/toop/request.php. It is highly recommended that ToO proposers register as Swift ToO users in advance at https://www.swift.psu.edu/secure/toop/too_newuser.php. 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 12 ToO proposals may be triggered until March 31, 2017."
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.
Prop PI Title
1215005 BODEWITS, DENNIS THE ACTIVITY AND EVOLUTION OF OORT CLOUD COMETS 1215013 BOGGS, STEVEN TOO OBSERVATION OF GRBS DETECTED WITH THE COSI BALLOON PAYLOAD 1215015 BOGDANOV, SLAVKO SWIFT MONITORING OF NEARBY X-RAY BINARY-RADIO MILLISECOND PULSAR TRANSITION OBJECTS 1215017 METZGER, BRIAN TESTING THE MAGNETAR MODEL FOR SUPERLUMINOUS SUPERNOVAE WITH SWIFT 1215023 KENNEA, JAMIE SWIFT LOCALIZATION OF MAXI DISCOVERED GALACTIC X-RAY TRANSIENTS 1215025 PERNA, ROSALBA SWIFT PRECURSORS TO LONG GRBS: HIDDEN SIGNS OF A NEWLY-BORN, HYPER-ACCRETING MAGNETAR? 1215055 STRADER, JAY THE COMPREHENSIVE VLA SURVEY FOR BLACK HOLES IN GLOBULAR CLUSTERS 1215059 SAND, DAVID EXPLOSION PHYSICS AND PROGENITORS FROM A ONE DAY CADENCE SUPERNOVA SEARCH 1215061 DEGENAAR, NATHALIE CONTINUING A SWIFT LEGACY: THE MONITORING CAMPAIGN OF THE GALACTIC CENTER 1215063 DEGENAAR, NATHALIE UNDERSTANDING THE CRUSTS OF TRANSIENTLY ACCRETING NEUTRON STARS 1215069 MEHDIPOUR, MISSAGH THE PURSUIT OF X-RAY OBSCURING OUTFLOWS IN AGN 1215074 FALCONE, ABE THE LARGEST FLARES FROM KNOWN TEV GAMMA RAY BLAZARS: SIMULTANEOUS OBSERVATIONS WITH TOOS 1215078 CENKO, STEPHEN UNVEILING THE PROGENITORS OF SHORT GAMMA-RAY BURSTS 1215082 WILLIAMS, DAVID TARGET OF OPPORTUNITY MULTIWAVELENGTH OBSERVATIONS OF NEW TEV BLAZARS 1215102 MARGUTTI, RAFFAELLA EXPLOSION MECHANISMS AND ENERGY SOURCES POWERING SUPER-LUMINOUS SUPERNOVAE 1215121 MILLER, JON SWIFT AND ASTRO-H OBSERVATIONS OF PERSISTENT BLACK HOLE X-RAY BINARIES 1215128 AGUEROS, MARCEL A SNAPSHOT SURVEY OF THE HYADES 1215150 PRITCHARD, TYLER DEEPER, WIDER, FASTER: HIGH ENERGY COUNTERPARTS TO THE FASTEST BURSTS IN THE SKY 1215151 CORSI, ALESSANDRA UNRAVELING THE PHYSICS OF BROAD-LINE TYPE IC SUPERNOVAE WITH ALMA+SWIFT 1215153 DELLER, ADAM REVEALING THE NATURE OF LOW-LEVEL ACCRETION IN AQL X-1 WITH SWIFT + VLA 1215154 LANDI, RAFFAELLA SWIFT/XRT FOLLOW-UP OBSERVATIONS OF UNIDENTIFIED INTEGRAL/IBIS SOURCES IN THE 1000 ORBIT CATALOGUE 1215158 SAKAMOTO, TAKANORI SWIFT RAPID FOLLOW-UP OBSERVATIONS OF MAXI XRFS 1215167 AJELLO, MARCO ON THE ORIGIN OF THE EXTRAGALACTIC GAMMA-RAY AND NEUTRINO BACKGROUNDS 1215176 PASHAM, DHEERAJ HIGH-CADENCE XRT MONITORING OF ULTRALUMINOUS X-RAY SOURCES TO SEARCH FOR ORBITAL PERIODS 1215179 LOHFINK, ANNE PROBING THE ACCRETION DISK SPECTRUM'S PEAK REGION 1215186 VESTRAND, W. THOMAS COLLECTING CRITICAL OPTICAL DIAGNOSTICS OF GAMMA-RAY BURSTS WITH THE RAPTOR TELESCOPES 1215188 MARGUTTI, RAFFAELLA PROBING THE MASS-LOSS HISTORY OF MASSIVE STARS WITH SWIFT 1215196 INSERRA, COSIMO SWIFT SURVEY FOR SUPER LUMINOUS SUPERNOVAE 1215199 GEZARI, SUVI CLEARING THE FOG: SYSTEMATIC SWIFT UV/X-RAY FOLLOW-UP OF IPTF NUCLEAR TRANSIENTS 1215203 CORSI, ALESSANDRA JOINT IPTF-VLA-SWIFT FOLLOW-UP OF ALIGO EVENTS 1215205 FOLEY, RYAN UV SPECTROSCOPY OF TYPE IA SUPERNOVAE 1215213 BROWN, PETER COMPLETING THE TEN YEAR SWIFT SUPERNOVA ARCHIVE WITH TEMPLATE OBSERVATIONS 1215215 JORSTAD, SVETLANA OPTICAL, UV, AND X-RAY DIPS IN THE RADIO GALAXY 3C 120 1215223 NELSON, THOMAS A COMPLEMENTARY RADIO AND X-RAY STUDY OF SHOCKS AND MASS EJECTION IN NOVAE 1215232 KASLIWAL, MANSI UNDERSTANDING YOUNG SUPERNOVAE & EXOTIC TRANSIENTS WITH SWIFT AND IPTF 1215235 KEIVANI, AZADEH SEEKING THE SOURCES OF THE HIGHEST-ENERGY COSMIC NEUTRINOS WITH SWIFT 1215238 MCHARDY, IAN SWIFT, KEPLER, HST AND GROUND BASED REVERBERATION MAPPING OF NGC4593: TEST OF ACCRETION DISC THEORY 1215240 VESTERGAARD, MARIANNE EFFECTS OF THE QUASAR SED ON BLACK HOLE MASS AND DISK WINDS 1215241 GALLO, ELENA THE RADIATIVE JET POWER OF QUIESCENT BLACK HOLE X-RAY BINARIES: CIRCUMBINARY DISK OR JET-DOMINATED ACCRETION? 1215255 FIELDS, BRIAN SWIFT ALERT, LOCALIZATION, AND FIRST LOOK AT A TYPE IA SUPERNOVA IN THE MILKY WAY 1215270 RANGELOV, BLAGOY REVEALING PULSARS HIDDEN IN THE 3RD FERMI CATALOG 1215280 OMODEI, NICOLA THE SWIFT DATA MINING PROJECT 1215281 LUNNAN, RAGNHILD UNVEILING SUPERLUMINOUS SUPERNOVAE WITH IPTF AND SWIFT
Prop |PI |Target_Num|Target_Name |Time [ ks ]|TOO|RA [ deg ]|Dec [ deg ]| 1215005|BODEWITS | 1 |C/2013 US10 CATALINA| 13.00 |N | 0.0000 | 0.0000 | 1215005|BODEWITS | 2 |C/2013 X1 PANSTARRS | 33.80 |N | 0.0000 | 0.0000 | 1215013|BOGGS | 1 |COSI GRB #1 | 70.00 |Y | 0.0000 | 0.0000 | 1215013|BOGGS | 2 |COSI GRB #2 | 70.00 |Y | 0.0000 | 0.0000 | 1215013|BOGGS | 3 |COSI GRB #3 | 70.00 |Y | 0.0000 | 0.0000 | 1215013|BOGGS | 4 |COSI GRB #4 | 70.00 |Y | 0.0000 | 0.0000 | 1215015|BOGDANOV | 1 |PSR J1023+0038 | 6.00 |N |155.9487 | 0.6448 | 1215015|BOGDANOV | 2 |XSS J12270-4859 | 6.00 |N |186.9948 |-48.8952 | 1215015|BOGDANOV | 3 |PSR J1723-2837 | 6.00 |N |260.8466 |-28.6325 | 1215015|BOGDANOV | 4 |J1628-3205 | 6.00 |N |247.0292 |-32.0969 | 1215015|BOGDANOV | 5 |PSR J2129-0429 | 6.00 |N |322.4375 | -4.4849 | 1215015|BOGDANOV | 6 |PSR J1816+4510 | 6.00 |N |274.1497 | 45.1761 | 1215015|BOGDANOV | 7 |PSR J2215+5135 | 6.00 |N |333.8862 | 51.5935 | 1215015|BOGDANOV | 8 |PSR J2339-0533 | 6.00 |N |354.9115 | -5.5515 | 1215015|BOGDANOV | 9 |1FGL J0523.5-2529 | 6.00 |N | 80.8205 |-25.4602 | 1215015|BOGDANOV | 10 |PSR J1417-4402 | 6.00 |N |214.3775 |-44.0493 | 1215015|BOGDANOV | 11 |3FGL J1544.6-1125 | 6.00 |N |236.1641 |-11.4679 | 1215023|KENNEA | 1 |MAXI TRANSIENT #1 | 1.00 |Y | 0.0000 | 0.0000 | 1215023|KENNEA | 2 |MAXI TRANSIENT #2 | 1.00 |Y | 0.0000 | 0.0000 | 1215023|KENNEA | 3 |MAXI TRANSIENT #3 | 1.00 |Y | 0.0000 | 0.0000 | 1215023|KENNEA | 4 |MAXI TRANSIENT #4 | 2.00 |Y | 0.0000 | 0.0000 | 1215023|KENNEA | 5 |MAXI TRANSIENT #5 | 2.00 |Y | 0.0000 | 0.0000 | 1215023|KENNEA | 6 |MAXI TRANSIENT #6 | 3.50 |Y | 0.0000 | 0.0000 | 1215023|KENNEA | 7 |MAXI TRANSIENT #7 | 5.00 |Y | 0.0000 | 0.0000 | 1215023|KENNEA | 8 |MAXI TRANSIENT #7 | 5.00 |Y | 0.0000 | 0.0000 | 1215059|SAND | 1 |SN_TOO_1 | 9.00 |Y | 0.0000 | 0.0000 | 1215059|SAND | 2 |SN_TOO_2 | 9.00 |Y | 0.0000 | 0.0000 | 1215059|SAND | 3 |SN_TOO_3 | 9.00 |Y | 0.0000 | 0.0000 | 1215061|DEGENAAR | 1 |GALACTIC CENTER |490.00 |N |266.4000 |-28.9833 | 1215063|DEGENAAR | 1 |QUIESCENT SOURCE | 50.00 |Y | 0.0000 | 0.0000 | 1215069|MEHDIPOUR | 1 |ARK 564 | 15.00 |N |340.6638 | 29.7254 | 1215069|MEHDIPOUR | 2 |MR 2251-178 | 10.00 |N |343.5242 |-17.5819 | 1215069|MEHDIPOUR | 3 |MRK 335 | 11.00 |N | 1.5816 | 20.2029 | 1215069|MEHDIPOUR | 4 |MRK 509 | 8.00 |N |311.0407 |-10.7234 | 1215069|MEHDIPOUR | 5 |MRK 841 | 13.00 |N |226.0049 | 10.4379 | 1215069|MEHDIPOUR | 6 |NGC 3783 | 15.00 |N |174.7572 |-37.7385 | 1215069|MEHDIPOUR | 7 |NGC 4593 | 11.00 |N |189.9145 | -5.3442 | 1215069|MEHDIPOUR | 8 |NGC 7469 | 13.00 |N |345.8153 | 8.8737 | 1215074|FALCONE | 1 |TEV BLAZAR | 10.00 |Y | 0.0000 | 0.0000 | 1215074|FALCONE | 2 |TEV BLAZAR | 10.00 |Y | 0.0000 | 0.0000 | 1215082|WILLIAMS | 1 |NEW VHE BLAZAR #1 | 15.00 |Y | 0.0000 | 0.0000 | 1215082|WILLIAMS | 2 |NEW VHE BLAZAR #2 | 15.00 |Y | 0.0000 | 0.0000 | 1215082|WILLIAMS | 3 |NEW VHE BLAZAR #3 | 15.00 |Y | 0.0000 | 0.0000 | 1215102|MARGUTTI | 1 |SLSN1 | 55.00 |Y | 0.0000 | 0.0000 | 1215102|MARGUTTI | 2 |SLSN2 | 55.00 |Y | 0.0000 | 0.0000 | 1215121|MILLER | 1 |GRS 1915+105 | 12.00 |N |288.7981 | 10.9458 | 1215121|MILLER | 2 |CYGNUS X-1 | 10.00 |N |299.5903 | 35.2016 | 1215128|AGUEROS | 1 |05030765+1343505 | 8.00 |N | 75.7818 | 13.7307 | 1215128|AGUEROS | 2 |04484211+2106035 | 7.00 |N | 72.1753 | 21.1011 | 1215128|AGUEROS | 3 |04360525+1541026 | 7.00 |N | 69.0219 | 15.6840 | 1215128|AGUEROS | 4 |04053965+1756156 | 7.00 |N | 61.4150 | 17.9378 | 1215128|AGUEROS | 5 |04083620+2346071 | 6.00 |N | 62.1509 | 23.7686 | 1215128|AGUEROS | 6 |04181926+1605181 | 7.00 |N | 64.5800 | 16.0884 | 1215128|AGUEROS | 7 |04241691+1800107 | 7.00 |N | 66.0703 | 18.0030 | 1215128|AGUEROS | 8 |04315244+1529585 | 12.00 |N | 67.9684 | 15.4995 | 1215128|AGUEROS | 9 |04052565+1926316 | 12.00 |N | 61.3567 | 19.4422 | 1215150|PRITCHARD | 1 |FRB/OPTICALTRANSIENT| 16.00 |Y | 0.0000 | 0.0000 | 1215151|CORSI | 1 |IPTF NEARBY BL-IC | 40.00 |Y | 0.0000 | 0.0000 | 1215153|DELLER | 1 |AQL X-1 | 14.00 |Y |287.8169 | 0.5849 | 1215154|LANDI | 1 |IGRJ01021+6612 | 5.00 |N | 15.5340 | 66.2100 | 1215154|LANDI | 2 |IGRJ01157+6941 | 5.00 |N | 18.8950 | 69.6890 | 1215154|LANDI | 3 |IGRJ01529-3531 | 5.00 |N | 28.2000 |-35.4950 | 1215154|LANDI | 4 |IGRJ02252+3748 | 5.00 |N | 36.3140 | 37.8020 | 1215154|LANDI | 5 |IGRJ02564-5232 | 5.00 |N | 44.1260 |-52.5330 | 1215154|LANDI | 6 |IGRJ03248-0223 | 5.00 |N | 51.2330 | -2.4030 | 1215154|LANDI | 7 |IGRJ04539+4502 | 5.00 |N | 73.4600 | 45.0380 | 1215154|LANDI | 8 |IGRJ05511-1218 | 5.00 |N | 87.7760 |-12.3220 | 1215154|LANDI | 9 |IGRJ07072-1227 | 5.00 |N |106.8010 |-12.4270 | 1215154|LANDI | 10 |IGRJ07541-3500 | 5.00 |N |118.5470 |-35.0080 | 1215154|LANDI | 11 |IGRJ08447+6610 | 5.00 |N |131.3560 | 66.1440 | 1215154|LANDI | 12 |IGRJ08507+1503 | 5.00 |N |132.6690 | 15.0540 | 1215154|LANDI | 13 |IGRJ13166+2340 | 5.00 |N |199.1320 | 23.6600 | 1215154|LANDI | 14 |IGRJ13216-5947 | 5.00 |N |200.4470 |-59.7660 | 1215154|LANDI | 15 |IGRJ14437-1653 | 5.00 |N |220.9380 |-16.8940 | 1215154|LANDI | 16 |IGRJ14557-5448 | 5.00 |N |223.8620 |-54.7860 | 1215154|LANDI | 17 |IGRJ15550-4034 | 5.00 |N |238.7710 |-40.5820 | 1215154|LANDI | 18 |IGRJ16476-3135 | 5.00 |N |251.8890 |-31.5570 | 1215154|LANDI | 19 |IGRJ16524-2352 | 5.00 |N |253.1220 |-23.8750 | 1215154|LANDI | 20 |IGRJ16565-1607 | 5.00 |N |254.1170 |-16.1200 | 1215154|LANDI | 21 |IGRJ17096-2036 | 5.00 |N |257.4150 |-20.6410 | 1215154|LANDI | 22 |IGRJ17116-3512 | 5.00 |N |257.9690 |-35.2200 | 1215154|LANDI | 23 |IGRJ17178-1859 | 5.00 |N |259.4890 |-18.9840 | 1215154|LANDI | 24 |IGRJ17193-3216 | 5.00 |N |259.8350 |-32.2740 | 1215154|LANDI | 25 |IGRJ17259+2603 | 5.00 |N |261.5210 | 25.9050 | 1215154|LANDI | 26 |IGRJ17385-3433 | 5.00 |N |264.6330 |-34.5490 | 1215154|LANDI | 27 |IGRJ18241-1456 | 5.00 |N |276.0380 |-14.9280 | 1215154|LANDI | 28 |IGRJ18497+5943 | 5.00 |N |282.4330 | 59.7160 | 1215154|LANDI | 29 |IGRJ19387-6502 | 5.00 |N |294.7410 |-65.0420 | 1215154|LANDI | 30 |IGRJ21095+4322 | 5.00 |N |317.3910 | 43.3460 | 1215154|LANDI | 31 |IGRJ21171+3930 | 5.00 |N |319.3060 | 39.5150 | 1215154|LANDI | 32 |IGRJ21304-1547 | 5.00 |N |322.6430 |-15.8110 | 1215154|LANDI | 33 |IGRJ21485+4306 | 5.00 |N |327.1270 | 43.1040 | 1215154|LANDI | 34 |IGRJ21540+4806 | 5.00 |N |328.4750 | 48.0850 | 1215154|LANDI | 35 |IGRJ11486-0505 | 5.00 |N |177.1600 | -5.0980 | 1215154|LANDI | 36 |IGRJ14300-2558 | 5.00 |N |217.5090 |-25.9820 | 1215154|LANDI | 37 |IGRJ17044-1844 | 5.00 |N |256.0890 |-18.7350 | 1215158|SAKAMOTO | 1 |MAXI XRF1_1 | 7.00 |Y | 0.0000 | 0.0000 | 1215158|SAKAMOTO | 2 |MAXI XRF1_2 | 4.00 |Y | 0.0000 | 0.0000 | 1215158|SAKAMOTO | 3 |MAXI XRF2_1 | 7.00 |Y | 0.0000 | 0.0000 | 1215158|SAKAMOTO | 4 |MAXI XRF2_2 | 4.00 |Y | 0.0000 | 0.0000 | 1215167|AJELLO | 1 |2FHL J1447.0-2658 | 5.00 |N |221.7620 |-26.9780 | 1215167|AJELLO | 2 |2FHL J2317.8+2838 | 5.00 |N |349.4660 | 28.6410 | 1215167|AJELLO | 3 |2FHL J1421.4-4447 | 5.00 |N |215.3690 |-44.7940 | 1215167|AJELLO | 4 |2FHL J1912.9-4456 | 5.00 |N |288.2250 |-44.9390 | 1215167|AJELLO | 5 |2FHL J2058.6-1832 | 5.00 |N |314.6570 |-18.5460 | 1215167|AJELLO | 6 |2FHL J0213.9-6949 | 5.00 |N | 33.4940 |-69.8170 | 1215167|AJELLO | 7 |2FHL J1635.4-1414 | 5.00 |N |248.8680 |-14.2420 | 1215167|AJELLO | 8 |2FHL J1147.0-1437 | 5.00 |N |176.7610 |-14.6300 | 1215167|AJELLO | 9 |2FHL J1136.5-2721 | 5.00 |N |174.1390 |-27.3540 | 1215167|AJELLO | 10 |2FHL J1155.5-3417 | 5.00 |N |178.8980 |-34.2990 | 1215167|AJELLO | 11 |2FHL J1427.7-3215 | 5.00 |N |216.9290 |-32.2660 | 1215176|PASHAM | 1 |NGC 5408 X-1 | 50.00 |N |210.8317 |-41.3829 | 1215176|PASHAM | 2 |NGC 55 ULX | 50.00 |N | 3.8704 |-39.2220 | 1215179|LOHFINK | 1 |PG 1247+267 |200.00 |N |192.5238 | 26.5188 | 1215188|MARGUTTI | 1 |IIN-SN1 | 49.00 |Y | 0.0000 | 0.0000 | 1215188|MARGUTTI | 2 |IIN-SN2 | 49.00 |Y | 0.0000 | 0.0000 | 1215196|INSERRA | 1 |SN2016XX | 19.00 |Y | 0.0000 | 0.0000 | 1215196|INSERRA | 2 |SN2016XY | 19.00 |Y | 0.0000 | 0.0000 | 1215196|INSERRA | 3 |SN2016YX | 19.00 |Y | 0.0000 | 0.0000 | 1215196|INSERRA | 4 |SN2016YY | 19.00 |Y | 0.0000 | 0.0000 | 1215196|INSERRA | 5 |SN2016ZZ | 19.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 1 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 2 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 3 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 4 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 5 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 6 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 7 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 8 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 9 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 10 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 11 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 12 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 13 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 14 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 15 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 16 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 17 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 18 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 19 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 20 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 21 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 22 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 23 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 24 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 25 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 26 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 27 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 28 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 29 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 30 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 31 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 32 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 33 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 34 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 35 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 36 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 37 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 38 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 39 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 40 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 41 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 42 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 43 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 44 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 45 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 46 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 47 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 48 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 49 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 50 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 51 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 52 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 53 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 54 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 55 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215199|GEZARI | 56 |IPTF16XXX | 2.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 1 |GWTRIGGER#1OPTCAND1 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 2 |GWTRIGGER#1OPTCAND2 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 3 |GWTRIGGER#1OPTCAND3 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 4 |GWTRIGGER#1OPTCAND4 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 5 |GWTRIGGER#1OPTCAND5 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 6 |GWTRIGGER#2OPTCAND1 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 7 |GWTRIGGER#2OPTCAND2 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 8 |GWTRIGGER#2OPTCAND3 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 9 |GWTRIGGER#2OPTCAND4 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 10 |GWTRIGGER#2OPTCAND5 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 11 |GWTRIGGER#3OPTCAND1 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 12 |GWTRIGGER#3OPTCAND2 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 13 |GWTRIGGER#3OPTCAND3 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 14 |GWTRIGGER#3OPTCAND3 | 3.00 |Y | 0.0000 | 0.0000 | 1215203|CORSI | 15 |GWTRIGGER#3OPTCAND3 | 3.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 1 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 2 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 3 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 4 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 5 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 6 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 7 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 8 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 9 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 10 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 11 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 12 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215205|FOLEY | 13 |SN1 | 15.00 |Y | 0.0000 | 0.0000 | 1215213|BROWN | 1 |NGC3287-SN13GE | 2.00 |N |158.6971 | 21.6483 | 1215213|BROWN | 2 |2MASSHOST-A14IL | 2.00 |N | 11.3856 |-14.2596 | 1215213|BROWN | 3 |NGC7610-SN13FS | 3.00 |N |349.9224 | 10.1850 | 1215213|BROWN | 4 |NGC337-SN14CX | 4.00 |N | 14.9587 | -7.5780 | 1215213|BROWN | 5 |HOST-LSQ14MO | 4.00 |N |155.6730 |-16.9207 | 1215213|BROWN | 6 |NGC4984-SN11IY | 3.00 |N |197.2385 |-15.5163 | 1215213|BROWN | 7 |NGC2466-A14DD | 32.00 |N |116.3169 |-71.4104 | 1215213|BROWN | 8 |UGC5623-SN | 3.00 |N |155.9525 | 33.8079 | 1215213|BROWN | 9 |UGC9379-SN13CU | 3.00 |N |218.4943 | 40.2444 | 1215213|BROWN | 10 |NGC2980-SN09LM | 4.00 |N |145.7999 | -9.6124 | 1215213|BROWN | 11 |MARK1309-SN14AD | 3.00 |N |179.4362 |-10.1730 | 1215213|BROWN | 12 |HOST-SN13HX | 6.00 |N | 23.8887 |-57.9641 | 1215213|BROWN | 13 |NGC3449-A15AJ | 3.00 |N |163.2236 |-32.9276 | 1215213|BROWN | 14 |2MAS-A14KD | 4.00 |N |343.3529 | 4.7994 | 1215213|BROWN | 15 |NGC4134-IPTF14AOI | 3.00 |N |182.2917 | 29.1769 | 1215213|BROWN | 16 |NGC5410-SN14AS | 2.00 |N |210.2275 | 40.9886 | 1215213|BROWN | 17 |NGC6951-SN15G | 2.00 |N |309.3087 | 66.1056 | 1215213|BROWN | 18 |M106-SN14BC | 2.00 |N |184.7396 | 47.3040 | 1215213|BROWN | 19 |SDSS-PTF11QCJ | 5.00 |N |198.4443 | 47.3050 | 1215213|BROWN | 20 |CGCG439-010-A15AR | 5.00 |N | 37.0903 | 10.3821 | 1215213|BROWN | 21 |UGC2789-SN13FV | 5.00 |N | 54.0565 | 67.5646 | 1215213|BROWN | 22 |NGC2748-SN | 2.00 |N |138.4292 | 76.4753 | 1215213|BROWN | 23 |NGC6908-SN | 5.00 |N |306.2874 |-24.8011 | 1215213|BROWN | 24 |NGC2196-SN | 3.00 |N | 93.0402 |-21.8059 | 1215213|BROWN | 25 |2MAS-LSQ13DDU | 5.00 |N | 59.7046 |-29.4200 | 1215213|BROWN | 26 |SDSS-SN13CV | 3.00 |N |245.6793 | 18.9594 | 1215213|BROWN | 27 |HOST-CSS14 | 5.00 |N |170.1542 | 30.4692 | 1215213|BROWN | 28 |KUG1237+183-A14AD | 5.00 |N |190.0475 | 18.0617 | 1215213|BROWN | 29 |PGC83768-SN12DA | 2.00 |N |195.6397 | 27.4365 | 1215213|BROWN | 30 |MRK884-A15FI | 2.00 |N |247.9529 | 20.4108 | 1215213|BROWN | 31 |NGC5112-SN | 3.00 |N |200.4850 | 38.7347 | 1215213|BROWN | 32 |NGC2668-SN | 3.00 |N |132.3440 | 36.7103 | 1215213|BROWN | 33 |NGC1448-SN14DF | 2.00 |N | 56.1330 |-44.6448 | 1215213|BROWN | 34 |SDSS-A14BU | 3.00 |N |169.6708 | 25.1665 | 1215213|BROWN | 35 |SDSS-A13DN | 2.00 |N |193.2425 | 32.4192 | 1215213|BROWN | 36 |UGC2653-SN07D | 3.00 |N | 49.6593 | 37.6081 | 1215213|BROWN | 37 |NGC4080-SN | 2.00 |N |181.2158 | 26.9925 | 1215213|BROWN | 38 |IC527-A14AR | 3.00 |N |137.4241 | 37.6016 | 1215213|BROWN | 39 |HOST-LSQ13CUW | 4.00 |N | 39.9890 | -8.5236 | 1215213|BROWN | 40 |HOST-SN08IY | 7.00 |N |242.1553 | 4.2741 | 1215213|BROWN | 41 |NGC4981-SN07C | 6.00 |N |197.2031 | -6.7775 | 1215213|BROWN | 42 |HOST-CSS081009 | 4.00 |N | 5.4625 |-16.5344 | 1215213|BROWN | 43 |HOST-PTF09ATU | 5.00 |N |247.6023 | 23.6403 | 1215213|BROWN | 44 |HOST-SN09JH | 4.00 |N |222.2922 | 29.4197 | 1215213|BROWN | 45 |MCG-01-10-39-SN13GD | 3.00 |N | 57.2728 | -3.0605 | 1215215|JORSTAD | 1 |3C120 |117.00 |N | 68.2963 | 5.3543 | 1215223|NELSON | 1 |NOVA TRIGGER 1 | 80.00 |Y | 0.0000 | 0.0000 | 1215223|NELSON | 2 |NOVA TRIGGER 2 | 80.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 1 |IPTFSWIFT1 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 2 |IPTFSWIFT2 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 3 |IPTFSWIFT3 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 4 |IPTFSWIFT4 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 5 |IPTFSWIFT5 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 6 |IPTFSWIFT6 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 7 |IPTFSWIFT7 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 8 |IPTFSWIFT8 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 9 |IPTFSWIFT9 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 10 |IPTFSWIFT10 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 11 |IPTFSWIFT11 | 5.00 |Y | 0.0000 | 0.0000 | 1215232|KASLIWAL | 12 |IPTFSWIFT12 | 5.00 |Y | 0.0000 | 0.0000 | 1215235|KEIVANI | 1 |HESE-1 MOSAIC | 19.00 |Y | 0.0000 | 0.0000 | 1215235|KEIVANI | 2 |HESE-2 MOSAIC | 19.00 |Y | 0.0000 | 0.0000 | 1215235|KEIVANI | 3 |HESE-3 MOSAIC | 19.00 |Y | 0.0000 | 0.0000 | 1215235|KEIVANI | 4 |HESE-1 SOURCE A | 6.00 |Y | 0.0000 | 0.0000 | 1215235|KEIVANI | 5 |HESE-1 SOURCE B | 6.00 |Y | 0.0000 | 0.0000 | 1215235|KEIVANI | 6 |HESE-2 SOURCE A | 6.00 |Y | 0.0000 | 0.0000 | 1215235|KEIVANI | 7 |HESE-2 SOURCE B | 6.00 |Y | 0.0000 | 0.0000 | 1215235|KEIVANI | 8 |HESE-3 SOURCE A | 6.00 |Y | 0.0000 | 0.0000 | 1215235|KEIVANI | 9 |HESE-3 SOURCE B | 6.00 |Y | 0.0000 | 0.0000 | 1215238|MCHARDY | 1 |NGC 4593 |212.00 |N |189.9145 | -5.3442 | 1215240|VESTERGAARD | 1 |Q0000-001 | 8.50 |N | 0.8758 | 0.1370 | 1215240|VESTERGAARD | 2 |Q0003-006 | 6.00 |N | 1.4437 | -0.4039 | 1215240|VESTERGAARD | 3 |Q0008-008 | 7.00 |N | 2.7123 | -0.5259 | 1215240|VESTERGAARD | 4 |Q0040-017 | 9.00 |N | 10.7304 | -1.4267 | 1215240|VESTERGAARD | 5 |Q0107-005 | 7.00 |N | 17.6021 | -0.2622 | 1215240|VESTERGAARD | 6 |Q0249-184 | 9.00 |N | 42.9501 |-18.2344 | 1215240|VESTERGAARD | 7 |Q0253-024 | 6.50 |N | 43.9169 | -2.2317 | 1215240|VESTERGAARD | 8 |Q0254-016 | 6.00 |N | 44.1683 | -1.4295 | 1215240|VESTERGAARD | 9 |Q0258+021 | 3.00 |N | 45.1917 | 2.3790 | 1215240|VESTERGAARD | 10 |Q0348+061 | 4.00 |N | 57.8188 | 6.3206 | 1215240|VESTERGAARD | 11 |Q2239+007 | 5.50 |N |340.5162 | 0.9876 | 1215240|VESTERGAARD | 12 |Q2351+022 | 6.00 |N |358.6265 | 2.5696 | 1215240|VESTERGAARD | 13 |Q0017+154 | 2.00 |N | 5.1051 | 15.6819 | 1215240|VESTERGAARD | 14 |Q0206+293 | 4.50 |N | 32.2861 | 29.5460 | 1215240|VESTERGAARD | 15 |Q0317-023 | 6.50 |N | 50.1197 | -2.1439 | 1215240|VESTERGAARD | 16 |Q0805+046 | 2.50 |N |121.9895 | 4.5427 | 1215240|VESTERGAARD | 17 |Q1606+289 | 7.50 |N |242.0466 | 28.8172 | 1215240|VESTERGAARD | 18 |Q1658+575 | 4.50 |N |254.9404 | 57.5251 | 1215240|VESTERGAARD | 19 |Q1701+379 | 7.50 |N |255.7832 | 37.8573 | 1215240|VESTERGAARD | 20 |J125140.83+080718.46| 6.00 |N |192.9200 | 8.1218 | 1215240|VESTERGAARD | 21 |J215543.09-073902.05| 8.00 |N |328.9300 | -7.6506 | 1215241|GALLO | 1 |V404 CYGNI | 15.00 |N |306.0160 | 33.8673 | 1215270|RANGELOV | 1 |3FGL J1624.1-4700 | 4.00 |N |246.0456 |-47.0027 | 1215270|RANGELOV | 2 |3FGL J2039.4+4111 | 4.00 |N |309.8573 | 41.1973 | 1215270|RANGELOV | 3 |3FGL J1456.7-6046 | 4.00 |N |224.2061 |-60.7773 | 1215270|RANGELOV | 4 |3FGL J2034.4+3833C | 4.00 |N |308.6200 | 38.5675 | 1215270|RANGELOV | 5 |3FGL J0839.6-4133 | 4.00 |N |129.9190 |-41.5528 | 1215270|RANGELOV | 6 |3FGL J0905.6-4917 | 4.00 |N |136.4199 |-49.2928 | 1215270|RANGELOV | 7 |3FGL J0915.8-5110 | 4.00 |N |138.9625 |-51.1803 | 1215270|RANGELOV | 8 |3FGL J0631.6+0644 | 4.00 |N | 97.9135 | 6.7397 | 1215270|RANGELOV | 9 |3FGL J1016.5-6034 | 4.00 |N |154.1482 |-60.5759 | 1215270|RANGELOV | 10 |3FGL J2024.6+3747 | 4.00 |N |306.1698 | 37.8022 | 1215270|RANGELOV | 11 |3FGL J1736.0-2701 | 4.00 |N |264.0205 |-27.0214 | 1215270|RANGELOV | 12 |3FGL J0704.1-1043 | 4.00 |N |106.0333 |-10.7283 | 1215270|RANGELOV | 13 |3FGL J0610.6+1728 | 4.00 |N | 92.6706 | 17.4722 | 1215270|RANGELOV | 14 |3FGL J1039.1-5809 | 4.00 |N |159.7883 |-58.1581 | 1215270|RANGELOV | 15 |3FGL J1729.5-2824 | 4.00 |N |262.3727 |-28.4084 | 1215270|RANGELOV | 16 |3FGL J0711.1-1037 | 4.00 |N |107.7975 |-10.6185 | 1215270|RANGELOV | 17 |3FGL J1037.2-6052 | 4.00 |N |159.3145 |-60.8777 | 1215270|RANGELOV | 18 |2FHL J2321.1+5910 | 4.00 |N |350.2858 | 59.1671 | 1215270|RANGELOV | 19 |2FHL J0826.1-4500 | 4.00 |N |126.5306 |-44.9989 | 1215281|LUNNAN | 1 |PTF-SLSN1 | 28.00 |Y | 0.0000 | 0.0000 | 1215281|LUNNAN | 2 |PTF-SLSN2 | 28.00 |Y | 0.0000 | 0.0000 |
1215005 / DENNIS BODEWITS / UNIVERSITY OF MARYLAND (COLLEGE PARK)
"THE ACTIVITY AND EVOLUTION OF OORT CLOUD COMETS"
We will investigate the effects of activity on cometary evolution, and to address which properties reflect comets' origins and which are products of subsequent processing. To do this we propose to use Swift UVOT to characterize the activity of two Oort cloud comets: one dynamically new, and one that passed the Sun before. We will use grism spectroscopy and photometric imaging to measure production rates of OH, dust, and minor species over the course of the apparitions. Our systematic sampling of the comets activity at different heliocentric distances will allow us to search for asymmetries around perihelion. Swift's unique capabilities will allow us determine the physical and chemical evolution of the comets' activity which can then be compared to that of other age classes of comets.
1215013 / STEVEN EDWARD BOGGS / UNIVERSITY OF CALIFORNIA (BERKELEY)
"TOO OBSERVATION OF GRBS DETECTED WITH THE COSI BALLOON PAYLOAD"
The Compton Spectrometer and Imager (COSI) is a wide-field, balloon-borne gamma-ray telescope (0.1-5 MeV) that will launch from New Zealand around April 1, 2016. The primary goal of this COSI flight is to perform pioneering measurements of gamma-ray polarization in GRBs to help probe the prompt emission mechanism and field geometry. On a ~50-day flight, we anticipate detecting around 8-10 GRBs and definitively measuring the polarization of ~4 GRBs. We are requesting Swift ToO observations of GRBs triggered by COSI with fluence levels high enough to permit measurement of the polarization. Swift observations will be crucial for enabling follow-up host galaxy and redshift determinations, as well as placing the polarization measurements in context of the afterglow properties.
1215015 / SLAVKO BOGDANOV / COLUMBIA UNIVERSITY
"SWIFT MONITORING OF NEARBY X-RAY BINARY-RADIO MILLISECOND PULSAR TRANSITION OBJECTS"
The recent 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 nascent 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 in the field of the Galaxy 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.
1215017 / BRIAN D METZGER / COLUMBIA UNIVERSITY
"TESTING THE MAGNETAR MODEL FOR SUPERLUMINOUS SUPERNOVAE WITH SWIFT"
The discovery of 'super-luminous' supernovae (SLSNe), with radiated energies ~ 10-100 times higher than normal SNe, indicates that massive stars end their lives in ways previously unanticipated. A popular model posits that SLSNe are powered by the magnetic spin-down a newly-born, rapidly-rotating magnetar. However, the magnetar model lacks a smoking gun observational prediction that would distinguish it from alternative scenarios. We will model the time evolution of nascent millisecond magnetar nebulae, in order to determine whether and when UV/X-ray radiation can ionize through the ejecta and escape to the observer (ionization break-out). Our results will allow us to translate UV/X-ray observations of SLSNe with Swift into a quantitative test of the magnetar model.
1215023 / JAMIE ALEXANDER 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 perform localization of Galactic X-ray Transients newly discovered by MAXI. MAXI scans almost the entire X-ray sky every ~91 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 0.5-20 keV energy band. Swift is able to provide rapid follow-up observations of MAXI triggers and localization up to 1.4 arc-second 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 will be used to provide astrometric corrections, and to search for any optical counterparts. Swift is proven to be uniquely capable in this task.
1215025 / ROSALBA PERNA / STATE UNIVERSITY OF NEW YORK AT STONY BROOK
"SWIFT PRECURSORS TO LONG GRBS: HIDDEN SIGNS OF A NEWLY-BORN, HYPER-ACCRETING MAGNETAR?"
Precursors to the prompt Gamma-ray Burst emission have arguably been one of the biggest surprises of the Swift satellite. They were not readily predicted by the collapsar model, and their interpretation still remains elusive. Among the various suggested scenarios, an accreting magnetar appears promising in explaining some of the main precursor features, by virtue of the strong dynamical coupling between its B-field lines and the accreting plasma. Here we propose to develop a quantitative model of this scenario, which computes the fallback mass accretion rate from numerical models of the collapsing envelope of the progenitor star, and generalizes the torque equations for magnetically-threaded disks to the hyper-accreting regime.
1215055 / JAY STRADER / MICHIGAN STATE UNIVERSITY
"THE COMPREHENSIVE VLA SURVEY FOR BLACK HOLES IN GLOBULAR CLUSTERS"
Spurred by our surprising VLA discovery of the first black holes in Milky Way globular clusters, we propose to continue our ambitious survey for both stellar-mass and intermediate-mass black holes in globular clusters. With well-defined selection criteria, our sample will allow the first statistical determination of the presence of black holes in clusters. This survey will make an immediate impact in a number of fields, including black hole demographics, accretion physics, gravitational wave predictions, and globular cluster evolution.
1215059 / DAVID SAND / TEXAS TECH UNIVERSITY
"EXPLOSION PHYSICS AND PROGENITORS FROM A ONE DAY CADENCE SUPERNOVA SEARCH"
In the early hours to days after explosion, supernovae (SNe) provide clues to how they explode, and what their progenitor star systems were. Motivated by the need to discover, and study, SNe within the first day of explosion, we have begun an NSF-funded one-day cadence SN search of nearby galaxies (D<40 Mpc), directly tied to robotic optical spectrographs for prompt followup. Our new survey will find ~2-3 SN Ia, ~2-3 SN Ib/c and ~5-6 SNII during the next Swift cycle, all within a day of explosion. The program will feed Swift young SN targets, and the resulting ultraviolet and X-ray data will put strong constraints on the progenitors of these nearby events.
1215061 / NATHALIE DEGENAAR / UNIVERSITY OF CAMBRIDGE
KEY PROJECT "CONTINUING A SWIFT LEGACY: THE MONITORING CAMPAIGN OF THE GALACTIC CENTER"
The center of our Galaxy has been monitored with the Swift/XRT almost every day since 2006. The high cadence provides excellent means to capture X-ray flares from Sgr A*, and to study the accretion properties of 14 nearby X-ray binaries. We propose to continue this Swift legacy program in cycles 12-13 and request daily 1-ks observations that amount to 490 ks of total exposure time. Our main objectives are to: 1) collect and study new flares from Sgr A*, 2) to test if the gaseous object G2 is disrupted and feeds matter to the supermassive black hole, and 3) to apply accretion models to very-faint X-ray binaries. This program is of high scientific value for a broad community.
1215063 / NATHALIE DEGENAAR / UNIVERSITY OF CAMBRIDGE
"UNDERSTANDING THE CRUSTS OF TRANSIENTLY ACCRETING NEUTRON STARS"
We propose 50 ks of ToO observations, spread over 25 pointings of 2 ks each, to monitor a transient neutron star X-ray binary as it transitions from outburst to quiescence. Studying how the accretion-heated crust of the neutron star cools after an outburst yields very valuable information about its structure and nuclear reactions occurring in a neutron-rich, high density environment. Investigating how much heat is generated in the outer crustal layers requires several temperature measurements within the first ~50 days of cooling. Swift is the key instrument to achieve this.
1215069 / MISSAGH MEHDIPOUR / SRON NETHERLANDS INSTITUTE FOR SPACE RESEARCH
"THE PURSUIT OF X-RAY OBSCURING OUTFLOWS IN AGN"
The recently discovered X-ray obscuring outflow in NGC 5548 is remarkably different from the commonly seen ionised outflows in AGN. It exhibits large columns of cold, high-velocity gas, close to the black hole and extending to the BLR. It produces broad UV absorption lines and shields much of the ionising radiation. This has important implications for the launching mechanism of the outflows. The extraordinary NGC 5548 finding was only made possible by combining the unique capabilities of Swift, XMM-Newton, HST and NuSTAR. We propose to extend our investigation to a sample of 8 suitable AGN to broaden our understanding of this phenomenon. We request weekly Swift monitoring of them in order to trigger joint XMM-Newton/HST/NuSTAR ToO observations. In total 96 ks of Swift time is requested.
1215074 / ABE D FALCONE / THE PENNSYLVANIA STATE UNIVERSITY
"THE LARGEST FLARES FROM KNOWN TEV GAMMA RAY BLAZARS: SIMULTANEOUS OBSERVATIONS WITH TOOS"
We propose to study known TeV blazars, most of which have never previously benefited from multiwavelength campaigns, during their highest flaring states. These proposed simultaneous multiwavelength observations will place severe constraints on the emission models. Simultaneous observations of X-ray, UV/optical, and gamma-ray emission during high states from these sources will provide the means to study relative flux, time delays, and the SED, thus enabling studies of particle acceleration and emission processes in blazar jets. Since the 1st peak of these SEDs is typically in the X-ray band and the 2nd peak is in the GeV/TeV band, Swift, VERITAS, and Fermi are ideal for these studies. The high flaring states required by the trigger criteria will ensure high science return.
1215078 / STEPHEN BRADLEY CENKO / NASA/GSFC
"UNVEILING THE PROGENITORS OF SHORT GAMMA-RAY BURSTS"
Despite tremendous progress in the last decade, an unambiguous link between short gamma-ray bursts (SGRBs) and their presumed progenitor systems, binary neutron star mergers, has remained elusive. Here we request funding to support our multi-wavelength campaign dedicated to the follow-up of Swift SGRBs, designed ultimately to directly identify their progenitor systems. Specifically, we focus on two questions: 1) What are the opening angles of Swift SGRBs (currently the dominant source of uncertainty in predicting detection rates for the Advanced LIGO and Virgo gravitational wave detectors)? 2) Can we detect the smoking gun "kilonova" signature to directly associate SGRBs with binary neutron star systems?
1215082 / DAVID A WILLIAMS / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)
"TARGET OF OPPORTUNITY MULTIWAVELENGTH OBSERVATIONS OF NEW TEV BLAZARS"
We propose target of opportunity observations of blazars showing strong evidence with VERITAS of being new very-high-energy gamma-ray sources. The known TeV blazars have spectral energy distributions with a synchrotron peak in the X-ray/UV/optical bands and a second peak at GeV energies, often thought to be inverse Compton emission. The VHE detection of a blazar often occurs when the blazar is in an active state, potentially lasting only a few days. Swift X-ray and UV observations during the discovery observations by VERITAS will probe the correlated flux and spectral variability patterns of the highest energy electrons. This will unveil information on the energetics and time scales of particle acceleration and cooling, critical to understanding the physics of jets in these new sources.
1215102 / RAFFAELLA MARGUTTI / NEW YORK UNIVERSITY
"EXPLOSION MECHANISMS AND ENERGY SOURCES POWERING SUPER-LUMINOUS SUPERNOVAE"
With bolometric peak luminosities L>7d43 erg/sec, the new class of Super Luminous Super Novae (SLSNe) outshine standard SN explosions of a factor ~10 and represent the death of the most massive stars in our Universe. Their exceptional luminosity requires exotic explosion mechanisms and/or sources of energy whose nature is unclear. Here we propose rapid Swift follow up of 2 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, XMM, 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.
1215121 / JON MILLER / UNIVERSITY OF MICHIGAN
"SWIFT AND ASTRO-H OBSERVATIONS OF PERSISTENT BLACK HOLE X-RAY BINARIES"
We request Swift observations of the variable but persistent Galactic black holes GRS 1915+105 and Cygnus X-1, simultaneously with early-phase Astro-H Performance and Verification observations of these sources. The excellent calibration of Swift, and the ability of the XRT to observe bright sources will make Swift observations essential to the success of initial high-resolution observations with Astro-H. In total, we request 22 ks of observing time, in 1 ks exposures.
1215128 / MARCEL AGUEROS / COLUMBIA UNIVERSITY
"A SNAPSHOT SURVEY OF THE HYADES"
Studies of stellar magnetic activity and rotation in young open clusters (<500 Myr) and field stars (2-10 Gyr) reveal the presence of a saturation threshold where activity no longer varies with rotation period (Prot). Measuring Prot and proxies for activity in older open clusters is difficult, but essential for understanding how the activity-rotation relation evolves. We propose a snapshot survey to complete the X-ray census of stars with measured Prot in the benchmark 650-Myr-old Hyades cluster. We have obtained new K2 data for 65 Hyads, bringing our catalog of Hyads with Prot to 134. By combining our X-ray and Prot data, we will analyze the behavior of coronal activity as a function of Rossby number at 650 Myr. We will compare these data to our Halpha data to test theories of saturation.
1215150 / TYLER A PRITCHARD / SWINBURNE UNIVERSITY OF TECHNOLOGY
"DEEPER, WIDER, FASTER: HIGH ENERGY COUNTERPARTS TO THE FASTEST BURSTS IN THE SKY"
Transient astrophysical phenomena have been continuously discovered as faster timescales have been probed. Recently, fast radio bursts (FRBs) have been discovered on millisecond timescales, which are likely extragalactic but whose physical mechanisms are unknown. In addition, minutes-to-hours time sampling have discovered optical counterparts to GRB's that once would have been thought to be optically dark and supernova discovery programs are pushing to shorter cadences in an effort to discover new transients such as kilonovae and shock breakouts. In a joint effort with the DECam on the CTIO-4m telescope, Parkes and Molongo radio observatories as part of the Deeper, Wider, Faster program we propose to use Swift to help identify high energy counterparts to FRB and fast optical transients.
1215151 / IRINA BORISOVNA VAVILOVA / NATIONAL ACADEMY OF SCIENCES OF UKRAINE
"X-RAY PROPERTIES OF THE LOW LUMINOSITY ISOLATED GALAXIES WITH ACTIVE NUCLEI Z <0.05"
The physical properties of isolated AGNs are poorly investigated especially in X-rays. Their study allows to separate the internal evolution mechanisms from the external influence of environment, and to consider them astwo separate processes related to fueling nuclear activity, forming the SMBH/accretion disk, and host galaxy morphology. Our sample of 61 isolated AGNs at z<0.05 was created by cross-matching the 2MIG catalogue with the Veron+2010 Catalogue. We note that only 21 isolated 2MIG AGNs have been observed with a good quality for their spectral analysis.The goals of this proposal are a) to perform the Swift observations for the sample of isolated AGNs, b)to explore both the X-ray continuum radiation from accretion disks around SMBHs and absorption line features.
1215153 / ADAM TRAVIS DELLER / ASTRON (NETHERLANDS FOUNDATION FOR RESEARCH IN ASTRONOMY)
"REVEALING THE NATURE OF LOW-LEVEL ACCRETION IN AQL X-1 WITH SWIFT + VLA"
Using Swift+VLA observations, we recently discovered that some neutron star binaries show surprisingly bright radio jets during low-level accretion (Deller et al. 2015). We see tentative indications that these "transitional" systems show a similar relationship between X-ray and radio luminosity as the well-studied black hole X-ray binaries, unlike the majority of neutron star binaries. Aql X-1 is one of the best-studied neutron star binaries, and exhibits some similarities to the transitional systems; by utilising simultaneous X-ray/radio observations for the first time at low accretion rates, we will extend simultaneous radio/X-ray observations over three orders of magnitude in X-ray luminosity and investigate the conditions required for powerful jet formation in neutron star binaries.
1215154 / RAFFAELLA LANDI / ISTITUTO DI ASTROFISICA SPAZIALE E FISICA COSMICA-BOLOGNA
"SWIFT/XRT FOLLOW-UP OBSERVATIONS OF UNIDENTIFIED INTEGRAL/IBIS SOURCES IN THE 1000 ORBIT CATALOGUE"
The last INTEGRAL/IBIS survey lists more than 200 hard X-ray sources which are unclassified, i.e. still lack arcsec location and consequently miss optical classification. The X-ray telescope on board Swift has proved to be a powerful tool to enhance the source localization (at the arcsec level) and, therefore, pinpoint the counterpart and provide optical spectroscopy. By combining XRT and IBIS data it is possible to study these sources over a wide energy band (typically 0.3-100 keV) and assess their spectral properties. Here, we propose to continue an on-going program of Swift/XRT follow-up observations of unidentified IBIS sources which has proved to be of tremendous importance in the discovery of the high-energy sky and an important legacy for future high-energy missions.
1215158 / TAKANORI SAKAMOTO / AOYAMA GAKUIN UNIVERSITY
"SWIFT RAPID FOLLOW-UP OBSERVATIONS OF MAXI XRFS"
We propose a Swift ToO program to observe XRFs 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. Furthermore, our program should also increase the number of redshift measurements of XRFs if the X-ray afterglow can be identified by Swift XRT. 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.
1215167 / MARCO AJELLO / CLEMSON UNIVERSITY
"ON THE ORIGIN OF THE EXTRAGALACTIC GAMMA-RAY AND NEUTRINO BACKGROUNDS"
Cosmic-ray interactions with ambient matter and radiation fields create high-energy neutrino and gamma-rays, thus establishing a link between the extragalactic gamma-ray background (EGB) measured by Fermi and the neutrino flux recently reported by IceCube. Star-forming galaxies are currently considered as candidates to explain the neutrino background and part of the EGB. Fermi's most recent survey above 50 GeV indicates that star-forming galaxies do not contribute substantially to either backgrounds. Thus, the gamma-ray and neutrino background might not have a common origin, unless there is, above 50 GeV, a non-neglibile population of sources other than blazars. Swift will test this hypothesis, by targeting half of the sample of unidentified >50 GeV sources that are visible from Chile.
1215176 / DHEERAJ RANGA REDDY PASHAM / NASA/GSFC
"HIGH-CADENCE XRT MONITORING OF ULTRALUMINOUS X-RAY SOURCES TO SEARCH FOR ORBITAL PERIODS"
We propose high-cadence XRT monitoring observations (1ksx5 visits per day for 10 days) of two variable, high-inclination ultraluminous X-ray sources (ULXs: NGC 5408 X-1 and NGC 55 ULX). Our main goal is to search for orbital periods in the range of a few 10s of hours in these two sources. This particular period range--typical of stellar-mass black hole binaries--has not been probed before. Any detected periods will be an important step towards dynamical mass measurement of these black holes. Swift, with its excellent X-ray sensitivity and fast maneuvering capability, is currently the only observatory that can carry out these observations. This proposal builds on previous successful Swift/XRT detection of a 12.1 hr orbital period from the ULX Holmberg IX X-1.
1215179 / ANNE MARIA LOHFINK / UNIVERSITY OF CAMBRIDGE
"PROBING THE ACCRETION DISK SPECTRUM'S PEAK REGION"
We propose to monitor the luminous quasar PG 1247+267 (z=2.038) for a duration of 150 days every 3 days with 4 ks Swift snapshots (200 ks total) to study its accretion disk. PG 1247+267's intermediate redshift allows us to probe further into UV (634-1446 A) than in any local AGN, letting us get a first snapshot of the peak region of the accretion disk spectrum with Swift and the inner regions around the black hole. Using UV lags and the UV rms spectrum, we will test the standard accretion disk model and confront recent claims of deviations from it.
1215186 / W. THOMAS VESTRAND / LOS ALAMOS NATIONAL LABORATORY
"COLLECTING CRITICAL OPTICAL DIAGNOSTICS OF GAMMA-RAY BURSTS WITH THE RAPTOR TELESCOPES"
We will explore the prompt and early afterglow optical emission from Swift-localized gamma ray bursts (GRBs) employing our RAPTOR (RAPid Telescopes for Optical Response) robotic telescopes. RAPTOR is a network of fast slewing telescopes with unique capabilities for collecting critical diagnostic measurements the optical emission during the first few minutes of the GRB. Our seven 0.4-meter rapid response telescopes will collect polarization, simultaneous 4-color (g r i z ) photometry, and high-cadence photometry starting <10 seconds after receipt of the Swift GRB localization. Those fast response measurements are complimented by observations from persistent monitors that cover the entire Swift field-of-view to search for bright emission before the response telescopes are on target.
1215188 / RAFFAELLA MARGUTTI / NEW YORK UNIVERSITY
"PROBING THE MASS-LOSS HISTORY OF 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 circum stellar medium interaction.
1215196 / COSIMO INSERRA / QUEEN'S UNIVERSITY BELFAST
"SWIFT SURVEY FOR SUPER LUMINOUS SUPERNOVAE"
In the last six years, a population of super-luminous supernovae has been identified, which have absolute magnitudes in the range -21 to -23. The discovery of these supernovae has been facilitated by the new generation of untargeted, wide-field optical surveys. These supernovae appear to occur preferentially in dwarf, metal-poor host galaxies but the cause of their extreme luminosity remains unknown. Theories include magnetar spin down, pair instability explosions, interaction of the SN ejecta with a massive circumstellar material or the fallback accretion onto a compact remnant. We propose to focus our ultraviolet follow-up and X-ray search at key epochs to measure their energetics and ultimately to constrain the progenitor channels.
1215199 / SUVI GEZARI / UNIVERSITY OF MARYLAND (COLLEGE PARK)
KEY PROJECT "CLEARING THE FOG: SYSTEMATIC SWIFT UV/X-RAY FOLLOW-UP OF IPTF NUCLEAR TRANSIENTS"
Nearly 50 years ago, theorists first proposed that an outburst of radiation from the tidal disruption of a star would be a unique signpost for a dormant supermassive black hole (SMBH) lurking in the center of a galaxy. With the now archetypal TDE candidate PS1-10jh, we demonstrated that time domain observations of TDEs can act not just as signposts, but also as cosmic scales to weigh SMBHs in distant galaxies. ZTF and LSST are poised to build up a statistically significant sample of TDE light curves to probe the demographics of SMBHs at cosmic distances. We propose a key project to perform a systematic Swift UV/X-ray follow-up of iPTF nuclear transients in order to train an efficient real-time classification engine for the ZTF and LSST era.
1215203 / ALESSANDRA CORSI / TEXAS TECH UNIVERSITY
"JOINT IPTF-VLA-SWIFT FOLLOW-UP OF ALIGO EVENTS"
Starting from 2015, a new window on the universe is going to open as the advanced ground-based Gravitational Wave (GW) detectors, aLIGO (now in its 1st observing run) and Virgo, will reach design sensitivity. Because GW-triggered events are expected to be only coarsely localized to large areas of the sky, the identification of electromagnetic counterparts could provide orders of magnitude better localization and enhance confidence in the GW detections. Here, we propose to complement our iPTF+VLA follow-up program of aLIGO triggers with data from Swift. A radio plus X-ray detection of the several optical candidates expected to be found in a typical GW trigger error-area would greatly enhance the confidence in the detection, and help identify the nature of the event.
1215205 / RYAN FOLEY / UNIVERSITY OF ILLINOIS AT URBANA-CHAMPAIGN
"UV SPECTROSCOPY OF TYPE IA SUPERNOVAE"
Type Ia supernovae (SN Ia) are incredibly useful distance indicators. However, we have identified a potential distance bias related to the progenitor star's metallicity. Thankfully, one can measure metallicity with UV spectroscopy. Unfortunately in addition to metallicity, other factors related to the explosion affect the UV spectra. To isolate metallicity effects, we must remove these other sources through empirical relations. Here we propose to build the statistical sample of SN Ia UV spectra necessary to measure these trends. This program will provide a lasting legacy for Swift, and in combination with HST data will further our understanding of SN Ia progenitor systems and explosions and improve SN Ia distance estimates.
1215213 / PETER J BROWN / TEXAS A&M UNIVERSITY
"COMPLETING THE TEN YEAR SWIFT SUPERNOVA ARCHIVE WITH TEMPLATE OBSERVATIONS"
The Swift Ultra-Violet/Optical Telescope (UVOT) has revolutionized the understanding of supernova (SN) behavior in the ultraviolet (UV). Swift has observed over 350 SNe, enabling detailed studies of individual objects, many of which were the first of their kind observed in the UV, and the differences within SN subgroups. These studies rely 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 45 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 and allow us to complete a catalog of data from the first ten years of Swift SN observations.
1215215 / SVETLANA G. JORSTAD / BOSTON UNIVERSITY
"OPTICAL, UV, AND X-RAY DIPS IN THE RADIO GALAXY 3C 120"
The investigators propose to monitor the radio galaxy 3C~120 with Swift over 2 years at optical-UV and X-ray bands in order to test two scenarios for the accretion disk/jet connection established by previous studies. One scenario predicts that the optical-UV spectral slope should steepen dramatically at the start of X-ray dips as the inner accretion disk (AD) vanishes. Under the other hypothesis, in which the X-ray emission occurs at the base of the jet, no such effect is expected. The resulting Swift observations will also provide a legacy dataset important for understanding the complex AD/corona/jet relationship.
1215223 / THOMAS NELSON / UNIVERSITY OF MINNESOTA
"A COMPLEMENTARY RADIO AND X-RAY STUDY OF SHOCKS AND MASS EJECTION IN NOVAE"
We propose to continue our multi-wavelength survey of nova outbursts, of which Swift XRT/UVOT are key components, augmented by radio, optical, infrared, and gamma-ray observations. Specifically, this program aims to explore how mass loss proceeds during nova outbursts using contemporaneous X-ray and VLA radio observations of up to two novae during the first year after discovery (160 ks request total). Together, the two regimes provide a complementary probe of the quantity, kinematics and structure of the ejected material. Understanding how mass is ejected in nova outbursts is crucial for determining the long term evolution of the white dwarfs in these systems and understanding the origin of GeV gamma-ray emission in novae.
1215232 / MANSI M. KASLIWAL / CALIFORNIA INSTITUTE OF TECHNOLOGY
"UNDERSTANDING YOUNG SUPERNOVAE & EXOTIC TRANSIENTS WITH SWIFT AND IPTF"
The intermediate Palomar Transient Factory (iPTF) operations are now in full swing with a focus on faster cadence and even more rapid response follow-up of optical transients. Our new software pipeline, building on the PTF legacy, regularly issues automated alerts for intra-night spectroscopic follow-up of extremely young supernovae. Here, we propose to continue our very productive Swift-iPTF program focused on young supernovae and fast evolving transients. UV observations have proved to be of unique value for the youngest supernovae. X-ray observations have played a key role in both identifying and understanding non-thermal sources. The proposed Swift-iPTF program will be complemented with aggressive multi-wavelength (ultra-rapid HST ToO, large Gemini, Palomar, Keck and EVLA) programs.
1215235 / AZADEH KEIVANI / THE PENNSYLVANIA STATE UNIVERSITY
"SEEKING THE SOURCES OF THE HIGHEST-ENERGY COSMIC NEUTRINOS WITH SWIFT"
We propose the first prompt searches for X-ray and UV/optical counterparts to IceCube high-energy (E >~ 30 TeV) likely-cosmic neutrinos with Swift. Using newly-installed high-energy event identification and reconstruction algorithms running at the South Pole, we will select up to three neutrinos with high probabilities of cosmic origin and good localizations. Each trigger will be observed with a mosaic of 19 Swift pointings, tilingthe neutrino localization to >50% completeness and 1 ks exposure within roughly 16 hours, in sequence designed to recover >50% of Swift GRB X-ray afterglows. Discovery of even a single EM counterpart to a high-energy neutrino would revolutionize our understanding of the source population, and potentially, reveal the origins of the highest-energy cosmic rays.
1215238 / IAN M MCHARDY / UNIVERSITY OF SOUTHAMPTON
KEY PROJECT "SWIFT, KEPLER, HST AND GROUND BASED REVERBERATION MAPPING OF NGC4593: TEST OF ACCRETION DISC THEORY"
Recent Swift monitoring of NGC5548 gave the best ever measurement of AGN X-ray/UV/optical interband lags, showing that UVOT short timescale variability is mostly due to reprocessing of X-rays by an accretion disc. However the lags are ~3x longer than expected from a standard Shakura-Sunyaev disc. There is something wrong with our understanding of accretion discs. Before speculating on the reason it is essential to measure lags of similar quality in AGN with different disc parameters. NGC4593, mass 7x less than NC5548 with guaranteed simultaneous daily HST, 3x daily griz and continuous Kepler observations to anchor the UVOT lags, is an outstanding candidate. These observations will also help understand the contribution of the BLR to UVOT variability. Only Swift can carry out this program.
1215240 / MARIANNE VESTERGAARD / UNIVERSITY OF ARIZONA
"EFFECTS OF THE QUASAR SED ON BLACK HOLE MASS AND DISK WINDS"
We ask for follow-up observations of 21 quasars with existing short Swift observations so to ensure a 3-4 sigma detection of the X-ray flux. These objects are part of a larger study of z~2 quasars. These additional data will increase by 60% our sample of X-ray detected quasars to 54 quasars. By combining new and existing Swift data with available radio maps and high-quality restframe UV-optical VLT spectra we will map and study how the ionizing spectral energy distribution affects the shape of the Hbeta, MgII, and CIV broad emission lines and thereby the black hole mass estimates in distant quasars. This study will also test recently proposed hypotheses of what determines the shape of broad emission lines and that intrinsic absorption lines take origin in quasar disk winds.
1215241 / ELENA GALLO / UNIVERSITY OF MICHIGAN
"THE RADIATIVE JET POWER OF QUIESCENT BLACK HOLE X-RAY BINARIES: CIRCUMBINARY DISK OR JET-DOMINATED ACCRETION?"
It is not clear whether quiescent black hole X-ray binaries (<1e-5 Ledd) liberate the bulk of their accretion power via an outflowing jet, orif it remains in the hot infalling gas. The answer heavily depends onthe frequency where the jet transitions from optically thick-to-thin(the so-called jet break). Here, we propose joint UVOT/XRT(15ks) and VLA(2h) observations of the black hole V404 Cygni to characterize the broadband spectrum above and below the jet break; these observations will be coordinated with the first mm observations (NOEMA) of any quiescent black hole X-ray binary. These data will allow us to place the best constraints on the jet spectral shape to date, thereby determining whether or not quiescent black holes are jet-dominated in terms of their overall power output.
1215255 / BRIAN FIELDS / UNIVERSITY OF ILLINOIS AT URBANA-CHAMPAIGN
"SWIFT ALERT, LOCALIZATION, AND FIRST LOOK AT A TYPE IA SUPERNOVA IN THE MILKY WAY"
Future Milky Way supernovae offer unique scientific opportunities, but likely explode ~10 kpc away in the Galactic plane and thus are optically dim. A Galactic Type Ia supernova will also be dim in the radio, X-ray, and neutrinos. Fortunately, Swift can detect Galactic SNIa events via the 158 keV gamma-ray line emitted in the radioactive decay of 56Ni to 56Co. Perhaps on the first day, this signal will rise above background in BAT, with line presenting a unique spectral signature. For ~1 day after discovery, Swift will be the only space-based telescope on target while others slew. We propose to model the ability of Swift to (1) detect this signal, (2) confirm its Type Ia origin, (3) localize the event for followup, and (4) constrain its properties via observations with the XRT and UVOT.
1215270 / BLAGOY RANGELOV / GEORGE WASHINGTON UNIVERSITY
"REVEALING PULSARS HIDDEN IN THE 3RD FERMI CATALOG"
We propose a survey of unclassified Fermi sources from the 3FGL and 2FHL catalogs. Using several parameter cuts, we have identified a sub-sample that will be dominated by pulsars with inclusion of high mass X-ray binaries (HMXBs), PWNe, and SNRs. We aim to identify their X-ray counterparts, thus increasing the population of galactic particle accelerators and, in particular, pulsars detected in both gamma-rays and X-rays. With this prudent shallow survey approach we will be able to identify new X-ray bright targets suitable for detailed follow-up studies with Chandra and XMM-Newton.
1215280 / NICOLA OMODEI / STANFORD UNIVERSITY
"THE SWIFT DATA MINING PROJECT"
We have developed a new, innovative framework based on machine-learning algorithms to analyze available catalog data and to provide a classification of the sources where is missing. The idea is simple: Classification Trees are trained on known objects, in order to predict the membership of a new object to a given class on the basis of its measured quantities. We propose to apply our methodology, already successfully applied to archival Fermi LAT data, to Swift surveys. We also plan to extend our analysis to the catalog of Swift GRBs applying data-mining algorithms to evaluate if intrinsic correlations between the variables exist. This could potentially provide a new method to estimate the cosmological redshift of the source and to intrinsically separate sub-classes of objects.
1215281 / RAGNHILD LUNNAN / CALIFORNIA INSTITUTE OF TECHNOLOGY
"UNVEILING SUPERLUMINOUS SUPERNOVAE WITH IPTF AND SWIFT"
Superluminous supernovae (SLSNe) are a rare class of transients with peak luminosities 10-100x those of ordinary SNe and unique spectra. Now a decade after their first discoveries (and even with (>50 objects found), fundamental questions like their energy sources and progenitors arestill unknown. One way to make progress is to focus on the low-redshift population, which can be studied in greater detail and to later times than their high-redshift counterparts. We propose to combine the discovery potential and follow-up resources of the Palomar Transient Factory with the UV time-domain capabilities of Swift to study two low-z SLSNe, allowing for a detailed comparison with progenitor models, and facilitating comparison with the growing number high-z SLSNe discovered.