Swift Cycle 14 Results
The lists below contain the proposals recommended by the Cycle 14 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 14 proposals for observation: Please note that the ROSES 2017 Appendix D.5 "Swift Guest Investigator Cycle 14" 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 14 ToO proposals may be triggered until March 31, 2019."
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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.
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Recommended Proposals
Prop PI Title Key Projects: 1417025 DEGENAAR, NATHALIE CONTINUING A SWIFT LEGACY: THE MONITORING CAMPAIGN OF THE GALACTIC CENTER 1417129 EDELSON, RICK INTENSIVE SWIFT/GROUND-BASED/HST ACCRETION DISK REVERBERATION MAPPING OF THE "BARE" ACTIVE GALACTIC NUCLEUS FAIRALL 9 1417181 BROWN, PETER SUPERNOVA KEY PROJECT: SWIFT RESPONSE TO NEARBY SUPERNOVAE 1417229 BARCLAY, THOMAS A COMPREHENSIVE, MULTI-WAVELENGTH SURVEY OF COOL STAR ACTIVITY 1417232 KENNEA, JAMIE KEY PROJECT: THE DETECTION AND MONITORING OF ELECTROMAGNETIC COUNTERPARTS OF GRAVITATIONAL WAVE SOURCES WITH SWIFT IN O3 Regular proposals: 1417018 GUIRIEC, SYLVAIN TESTING A NEW MODEL FOR GRB PROMPT EMISSION FROM OPTICAL TO GAMMA-RAYS AND EXPLORING GRBS AS STANDARD CANDLES 1417019 MEHDIPOUR, MISSAGH CHASING OBSCURING WINDS WITH SWIFT 1417037 HENZE, MARTIN PROBING THE ERUPTION STATISTICS AND EVOLUTION OF THE UNIQUE RECURRENT NOVA M31N 2008-12A 1417043 BERGER, EDO UNIQUE INSIGHTS INTO SWIFT GRBS WITH THE VLA AND ALMA 1417057 VAN DEN EIJNDEN, JAKOB THE NATURE AND ACCRETION FLOW PROPERTIES OF SUB-LUMINOUS X-RAY BINARIES 1417063 AJELLO, MARCO TOWARDS THE FULL IDENTIFICATION OF THE 3FHL CATALOG 1417065 BODEWITS, DENNIS ROTATION AND CHEMICAL HETEROGENEITY OF HYPERACTIVE COMET 46P/WIRTANEN 1417070 HAIMAN, ZOLTAN TESTING THE ORIGIN OF PERIODIC VARIABILITY FOR THE BINARY CANDIDATE QUASAR PG1302-102 1417094 FILIPPENKO, ALEXEI GROUND-BASED OPTICAL STUDIES OF SWIFT GAMMA-RAY BURSTS, CYCLE 14 1417098 HERVET, OLIVIER PROBING A SCENARIO OF MULTIPLE RECOLLIMATION SHOCKS IN THE BL LAC MRK 421 1417106 KEIVANI, AZADEH SEEKING THE SOURCES OF THE HIGHEST-ENERGY COSMIC NEUTRINOS WITH SWIFT 1417122 KARA, ERIN TESTING THE ULX UNIFIED MODEL WITH SWIFT MONITORING OF NGC 6946 X-1 1417132 HOLDER, JAMIE COMPLETE PERIASTRON COVERAGE OF THE 50-YEAR BINARY PSR J2032+4127/ MT91~213. 1417134 SALZ, MICHAEL PROBING THE MASS LOSS OF THE HOTTEST GAS PLANEST 1417137 NEILL, JAMES ROBOTIC SPECTROSCOPIC FOLLOWUP OF SWIFT GRBS 1417138 MARGUTTI, RAFFAELLA DETAILED MAPPING OF EXTREME MASS-LOSS FROM EVOLVED MASSIVE STARS WITH SWIFT 1417139 CACKETT, EDWARD ACCRETION DISK REVERBERATION MAPPING OF A SUPER-EDDINGTON AGN 1417151 ZEZAS, ANDREAS REVEALING THE TRANSIENT X-RAY BINARY POPULATION OF THE LMC 1417156 PASHAM, DHEERAJ XRT AND UVOT MONITORING OF THE TIDAL DISRUPTION FLARE ASASSN-14LI TO DETECT THE NEWLY FORMED ACCRETION DISK 1417159 VESTERGAARD, MARIANNE TOO MONITORING OF THE RE-AWAKENING AGN IN MRK590: CATCHING THE MONSTER IN THE ACT! 1417168 VESTERGAARD, MARIANNE MONITORING THE SLEEPING MONSTER IN AGN MRK590 AND CLUES TO THE NATURE OF ITS RADIO EMISSION 1417179 FUERST, FELIX SWIFT MONITORING OF NEUTRON STAR POWERED ULTRA-LUMINOUS X-RAY SOURCES 1417202 HAGEN, LEA MODELING THE PHYSICAL PARAMETERS AND ULTRAVIOLET DUST EXTINCTION CURVE IN FIVE NEARBY DWARF GALAXIES 1417210 HOMAN, JEROEN A RARE LOOK AT A BLACK HOLE TRANSIENT EMERGING FROM QUIESCENCE Fill-Ins: 1417036 MARCHESI, STEFANO THE LEGACY OF SWIFT-BAT: THE TALE OF AGN AT HARD X-RAYS
Recommended Targets
Definition of Columns
- Proposal: Proposal number assigned by Swift mission
- PI: Principal Investigator's last name
- Target_Num: Target number as listed on the proposal form
- Target_Name: Target name as listed on proposal forms
- RA: Right Ascension (equinox J2000) in degrees
- Dec: Declination (equinox J2000) in degrees
- Time: Total observing time approved, in ksec
- ToO: "Y" if Target of Opportunity proposal, otherwise "N"
Prop |PI |Target_Num|Target_Name |Time [ ks ]|TOO|RA [ deg ]|Dec [ deg ]| 1417025|DEGENAAR | 1 |GALACTIC CENTER | 490.00 |N |266.4000 |-28.9833 | 1417129|EDELSON | 1 |FAIRALL 9 | 325.00 |N | 20.9405 |-58.8058 | 1417181|BROWN | 1 |SN_1 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 2 |SN_2 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 3 |SN_3 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 4 |SN_4 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 5 |SN_5 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 6 |SN_6 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 7 |SN_7 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 8 |SN_8 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 9 |SN_9 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 10 |SN_10 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 11 |SN_11 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 12 |SN_12 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 13 |SN_13 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 14 |SN_14 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 15 |SN_15 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 16 |SN_16 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 17 |SN_17 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 18 |SN_18 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 19 |SN_19 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 20 |SN_20 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 21 |SN_21 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 22 |SN_22 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 23 |SN_23 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 24 |SN_24 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 25 |SN_25 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 26 |SN_26 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 27 |SN_27 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 28 |SN_28 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 29 |SN_29 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 30 |SN_30 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 31 |SN_31 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 32 |SN_32 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 33 |SN_33 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 34 |SN_34 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 35 |SN_35 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 36 |SN_36 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 37 |SN_37 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 38 |SN_38 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 39 |SN_39 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 40 |SN_40 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 41 |SN_41 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 42 |SN_42 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 43 |SN_43 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 44 |SN_44 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 45 |SN_45 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 46 |SN_46 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 47 |SN_47 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 48 |SN_48 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 49 |SN_49 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 50 |SN_50 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 51 |SN_51 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 52 |SN_52 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 53 |SN_53 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 54 |SN_54 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 55 |SN_55 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 56 |SN_56 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 57 |SN_57 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 58 |SN_58 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 59 |SN_59 | 12.00 |Y | 0.0000 | 0.0000 | 1417181|BROWN | 60 |SN_60 | 12.00 |Y | 0.0000 | 0.0000 | 1417229|BARCLAY | 1 |PROXIMA CEN | 40.00 |N |217.4290 |-62.6795 | 1417229|BARCLAY | 2 |GJ 3136 | 40.00 |N | 32.2234 | 49.4490 | 1417229|BARCLAY | 3 |BD+01_2447 | 40.00 |N |157.2315 | 0.8410 | 1417229|BARCLAY | 4 |BARNARD'S STAR | 40.00 |N |269.4521 | 4.6934 | 1417229|BARCLAY | 5 |AU MIC | 40.00 |N |311.2897 |-31.3409 | 1417229|BARCLAY | 6 |LACAILLE 9352 | 40.00 |N |346.4668 |-35.8531 | 1417229|BARCLAY | 7 |UV CET | 40.00 |N | 24.7564 |-17.9501 | 1417229|BARCLAY | 8 |TWA22A | 40.00 |N |154.3620 |-53.9074 | 1417229|BARCLAY | 9 |WOLF 1061 | 40.00 |N |247.5753 |-12.6626 | 1417229|BARCLAY | 10 |WW PSA | 40.00 |N |341.2415 |-33.2505 | 1417229|BARCLAY | 11 |AX MIC | 40.00 |N |319.3136 |-38.8674 | 1417229|BARCLAY | 12 |HIP 23309 | 40.00 |N | 75.1964 |-57.2571 | 1417229|BARCLAY | 13 |NLTT 33370 | 40.00 |N |198.5850 | 13.3337 | 1417229|BARCLAY | 14 |LHS 292 | 40.00 |N |162.0524 |-11.3356 | 1417229|BARCLAY | 15 |FOMALHAUT C | 40.00 |N |342.0186 |-24.3687 | 1417229|BARCLAY | 16 |LUYTEN'S STAR | 40.00 |N |111.8521 | 5.2258 | 1417229|BARCLAY | 17 |V1005 ORI | 40.00 |N | 74.8951 | 1.7835 | 1417229|BARCLAY | 18 |LALANDE 21185 | 40.00 |N |165.8341 | 35.9699 | 1417229|BARCLAY | 19 |HD 82443B | 40.00 |N |143.2011 | 26.9956 | 1417229|BARCLAY | 20 |WOLF 424 | 40.00 |N |188.3224 | 9.0211 | 1417229|BARCLAY | 21 |AD LEO | 40.00 |N |154.9012 | 19.8700 | 1417229|BARCLAY | 22 |GJ 1284 | 40.00 |N |352.5560 |-20.3910 | 1417229|BARCLAY | 23 |KAPTEYN'S STAR | 40.00 |N | 77.9191 |-45.0184 | 1417229|BARCLAY | 24 |ROSS 248 | 40.00 |N |355.4791 | 44.1780 | 1417229|BARCLAY | 25 |AP COL | 40.00 |N | 91.2173 |-34.5601 | 1417229|BARCLAY | 26 |GJ 581 | 40.00 |N |229.8618 | -7.7223 | 1417229|BARCLAY | 27 |GJ 205 | 40.00 |N | 82.8642 | -3.6772 | 1417229|BARCLAY | 28 |DX CNC | 40.00 |N |127.4556 | 26.7760 | 1417229|BARCLAY | 29 |NLTT 31625 | 40.00 |N |190.6646 |-36.3419 | 1417229|BARCLAY | 30 |EQ PEG | 40.00 |N |352.9674 | 19.9373 | 1417229|BARCLAY | 31 |GLIESE 832 | 40.00 |N |323.3916 |-49.0090 | 1417229|BARCLAY | 32 |GJ 1061 | 40.00 |N | 53.9987 |-44.5126 | 1417229|BARCLAY | 33 |GJ 82 | 40.00 |N | 29.8480 | 58.5211 | 1417229|BARCLAY | 34 |YZ CMI | 40.00 |N |117.4687 |-17.4274 | 1417229|BARCLAY | 35 |GLIESE 1 | 40.00 |N | 1.3518 |-37.3574 | 1417229|BARCLAY | 36 |EZ AQR | 40.00 |N |339.6405 |-15.2993 | 1417229|BARCLAY | 37 |LP 776-25 | 40.00 |N | 73.1017 |-16.8227 | 1417229|BARCLAY | 38 |GJ 674 | 40.00 |N |262.1664 |-46.8952 | 1417229|BARCLAY | 39 |HIP 17695 | 40.00 |N | 56.8473 | -1.9722 | 1417229|BARCLAY | 40 |YZ CET | 40.00 |N | 18.1277 |-16.9990 | 1417229|BARCLAY | 41 |GLIESE 15A | 40.00 |N | 4.5954 | 44.0229 | 1417229|BARCLAY | 42 |UCAC4 516-086171 | 40.00 |N |282.9985 | 13.0010 | 1417229|BARCLAY | 43 |GLIESE 876 | 40.00 |N |343.3197 |-14.2637 | 1417229|BARCLAY | 44 |GJ 4353 | 40.00 |N |354.5726 |-41.5177 | 1417229|BARCLAY | 45 |GLIESE 725 | 40.00 |N |280.6946 | 59.6304 | 1417232|KENNEA | 1 |GW EM CANDIDATE #1 | 70.00 |Y | 0.0000 | 0.0000 | 1417232|KENNEA | 2 |GW EM CANDIDATE #2 | 70.00 |Y | 0.0000 | 0.0000 | 1417232|KENNEA | 3 |GW EM CANDIDATE #3 | 70.00 |Y | 0.0000 | 0.0000 | 1417019|MEHDIPOUR | 1 |ARK 564 | 15.00 |N |340.6638 | 29.7254 | 1417019|MEHDIPOUR | 2 |MR 2251-178 | 14.00 |N |343.5242 |-17.5819 | 1417019|MEHDIPOUR | 3 |MRK 509 | 12.00 |N |311.0407 |-10.7234 | 1417019|MEHDIPOUR | 4 |MRK 841 | 15.00 |N |226.0049 | 10.4379 | 1417019|MEHDIPOUR | 5 |NGC 3227 | 14.00 |N |155.8774 | 19.8651 | 1417019|MEHDIPOUR | 6 |NGC 4593 | 14.00 |N |189.9145 | -5.3442 | 1417019|MEHDIPOUR | 7 |NGC 7469 | 14.00 |N |345.8153 | 8.8737 | 1417037|HENZE | 1 |M31N 2008-12A | 84.00 |Y | 11.3704 | 41.9028 | 1417057|VAN DEN EIJNDEN | 1 |VFXT | 30.00 |Y | 0.0000 | 0.0000 | 1417063|AJELLO | 1 |3FHL J1036.3-5833 | 4.00 |N |159.0940 |-58.5630 | 1417063|AJELLO | 2 |3FHL J1652.2-4633 | 4.00 |N |253.0550 |-46.5560 | 1417063|AJELLO | 3 |3FHL J0531.8-6639 | 4.00 |N | 82.9700 |-66.6500 | 1417063|AJELLO | 4 |3FHL J0500.9-6945 | 4.00 |N | 75.2500 |-69.7500 | 1417063|AJELLO | 5 |3FHL J1655.5-4737 | 4.00 |N |253.8830 |-47.6320 | 1417063|AJELLO | 6 |3FHL J1830.0-1518 | 4.00 |N |277.5070 |-15.3013 | 1417063|AJELLO | 7 |3FHL J1855.3+0751 | 4.00 |N |283.8350 | 7.8665 | 1417063|AJELLO | 8 |3FHL J0057.9+6325 | 4.00 |N | 14.4862 | 63.4236 | 1417063|AJELLO | 9 |3FHL J1439.9-3955 | 4.00 |N |219.9990 |-39.9282 | 1417063|AJELLO | 10 |3FHL J1648.1-1548 | 4.00 |N |252.0360 |-15.8037 | 1417063|AJELLO | 11 |3FHL J0929.2-4110 | 4.00 |N |142.3250 |-41.1694 | 1417063|AJELLO | 12 |3FHL J0648.3+1744 | 4.00 |N |102.0790 | 17.7471 | 1417063|AJELLO | 13 |3FHL J0359.4-0235 | 4.00 |N | 59.8679 | -2.5876 | 1417063|AJELLO | 14 |3FHL J0933.5-5240 | 4.00 |N |143.3880 |-52.6714 | 1417063|AJELLO | 15 |3FHL J1048.4-5030 | 4.00 |N |162.1040 |-50.5125 | 1417063|AJELLO | 16 |3FHL J0528.4+3851 | 4.00 |N | 82.1220 | 38.8605 | 1417063|AJELLO | 17 |3FHL J1451.8-4145 | 4.00 |N |222.9530 |-41.7624 | 1417063|AJELLO | 18 |3FHL J1719.0-5348 | 4.00 |N |259.7630 |-53.8098 | 1417063|AJELLO | 19 |3FHL J0233.5+0657 | 4.00 |N | 38.3842 | 6.9576 | 1417063|AJELLO | 20 |3FHL J2239.5-2439 | 4.00 |N |339.8930 |-24.6536 | 1417065|BODEWITS | 1 |COMET 46P/WIRTANEN | 28.00 |N | 0.0000 | 0.0000 | 1417070|HAIMAN | 1 |PKS1302-102 | 21.00 |N |196.3875 |-10.5554 | 1417098|HERVET | 1 |MRK 421 | 60.00 |Y |166.1138 | 38.2088 | 1417106|KEIVANI | 1 |NEUTRINO-1 MOSAIC | 19.00 |Y | 0.0000 | 0.0000 | 1417106|KEIVANI | 2 |NEUTRINO-2 MOSAIC | 7.00 |Y | 0.0000 | 0.0000 | 1417106|KEIVANI | 3 |NEUTRINO-3 MOSAIC | 7.00 |Y | 0.0000 | 0.0000 | 1417106|KEIVANI | 4 |NEUTRINO-4 MOSAIC | 7.00 |Y | 0.0000 | 0.0000 | 1417106|KEIVANI | 5 |NEUTRINO-1 SOURCE A | 4.00 |Y | 0.0000 | 0.0000 | 1417106|KEIVANI | 6 |NEUTRINO-1 SOURCE B | 4.00 |Y | 0.0000 | 0.0000 | 1417106|KEIVANI | 7 |NEUTRINO-2 SOURCE A | 4.00 |Y | 0.0000 | 0.0000 | 1417106|KEIVANI | 8 |NEUTRINO-3 SOURCE A | 4.00 |Y | 0.0000 | 0.0000 | 1417106|KEIVANI | 9 |NEUTRINO-4 SOURCE A | 4.00 |Y | 0.0000 | 0.0000 | 1417122|KARA | 1 |NGC 6946 X-1 | 73.00 |N |308.7531 | 60.1918 | 1417132|HOLDER | 1 |PSR J2032+4127 | 72.00 |N |308.0547 | 41.4568 | 1417134|SALZ | 1 |HAT-P-67 | 25.20 |N |256.6107 | 44.7770 | 1417134|SALZ | 2 |WASP-76 | 28.80 |N | 26.6328 | 2.7006 | 1417134|SALZ | 3 |KELT-11 | 25.20 |N |161.7072 | -9.3990 | 1417134|SALZ | 4 |WASP-82 | 21.60 |N | 72.6607 | 1.8939 | 1417134|SALZ | 5 |WASP-79 | 28.80 |N | 66.3709 |-30.6004 | 1417134|SALZ | 6 |WASP-18 | 28.80 |N | 24.3543 |-45.6779 | 1417138|MARGUTTI | 1 |SNINTERACTING1 | 49.00 |Y | 0.0000 | 0.0000 | 1417138|MARGUTTI | 2 |SNINTERACTING2 | 49.00 |Y | 0.0000 | 0.0000 | 1417139|CACKETT | 1 |MRK 142 | 180.00 |N |156.3804 | 51.6764 | 1417151|ZEZAS | 1 |LMC FIELD 1 |3750.00 |N | 82.4354 |-69.7072 | 1417151|ZEZAS | 2 |LMC FIELD 2 |3750.00 |N | 81.5687 |-69.6306 | 1417151|ZEZAS | 3 |LMC FIELD 3 |3750.00 |N | 80.7592 |-69.6083 | 1417151|ZEZAS | 4 |LMC FIELD 4 |3750.00 |N | 79.9550 |-69.5806 | 1417151|ZEZAS | 5 |LMC FIELD 5 |3750.00 |N | 79.0958 |-69.5472 | 1417151|ZEZAS | 6 |LMC FIELD 6 |3750.00 |N | 82.1887 |-69.4194 | 1417151|ZEZAS | 7 |LMC FIELD 7 |3750.00 |N | 81.3125 |-69.3569 | 1417151|ZEZAS | 8 |LMC FIELD 8 |3750.00 |N | 80.4917 |-69.3500 | 1417151|ZEZAS | 9 |LMC FIELD 9 |3750.00 |N | 79.6050 |-69.3236 | 1417151|ZEZAS | 10 |LMC FIELD 10 |3750.00 |N | 78.7583 |-69.3569 | 1417151|ZEZAS | 11 |LMC FIELD 11 |3750.00 |N | 82.6554 |-69.1472 | 1417151|ZEZAS | 12 |LMC FIELD 12 |3750.00 |N | 83.8187 |-65.5889 | 1417151|ZEZAS | 13 |LMC FIELD 13 |3750.00 |N | 83.0396 |-65.5861 | 1417151|ZEZAS | 14 |LMC FIELD 14 |3750.00 |N | 83.3542 |-65.8444 | 1417151|ZEZAS | 15 |LMC FIELD 15 |3750.00 |N | 82.6458 |-65.8250 | 1417151|ZEZAS | 16 |LMC FIELD 16 |3750.00 |N | 82.7292 |-66.0194 | 1417151|ZEZAS | 17 |LMC FIELD 17 |3750.00 |N | 83.8137 |-66.9181 | 1417151|ZEZAS | 18 |LMC FIELD 18 |3750.00 |N | 82.9104 |-66.8806 | 1417151|ZEZAS | 19 |LMC FIELD 19 |3750.00 |N | 82.5225 |-67.1000 | 1417151|ZEZAS | 20 |LMC FIELD 20 |3750.00 |N | 77.1417 |-68.4472 | 1417151|ZEZAS | 21 |LMC FIELD 21 |3750.00 |N | 76.9104 |-68.7417 | 1417151|ZEZAS | 22 |LMC FIELD 22 |3750.00 |N | 72.9542 |-69.8139 | 1417151|ZEZAS | 23 |LMC FIELD 23 |3750.00 |N | 73.7646 |-69.9278 | 1417151|ZEZAS | 24 |LMC FIELD 24 |3750.00 |N | 73.9779 |-70.2181 | 1417151|ZEZAS | 25 |LMC FIELD 25 |3750.00 |N | 73.3258 |-69.2389 | 1417156|PASHAM | 1 |ASASSN-14LI | 48.00 |N |192.0635 | 17.7739 | 1417159|VESTERGAARD | 1 |MRK 590 | 130.00 |Y | 33.6399 | -0.7668 | 1417168|VESTERGAARD | 1 |MRK 590 | 48.00 |N | 33.6399 | -0.7668 | 1417179|FUERST | 1 |NGC 5907 ULX1 | 52.00 |N |228.9957 | 56.3030 | 1417179|FUERST | 2 |NGC 7793 P13 | 41.00 |N |359.4625 |-32.6241 | 1417202|HAGEN | 1 |NGC6503-D1 | 15.00 |N |268.2017 | 70.1373 | 1417202|HAGEN | 2 |ERIDANUS-3 | 25.00 |N | 35.6897 |-52.2837 | 1417202|HAGEN | 3 |RETICULUM-2 | 25.00 |N | 53.9256 |-54.0492 | 1417202|HAGEN | 4 |GALFA-DW3 | 20.00 |N | 44.7343 | 13.6297 | 1417202|HAGEN | 5 |GALFA-DW4 | 20.00 |N | 86.4366 | 10.7710 | 1417210|HOMAN | 1 |H1743-322 | 43.00 |N |266.5650 |-32.2335 |
Proposal Abstracts
1417025 / NATHALIE DEGENAAR / UNIVERSITEIT VAN AMSTERDAM
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 16 transient
X-ray binaries. We propose to continue this Swift legacy program in cycles
14-15 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.
1417129 / RICK EDELSON / UNIVERSITY OF MARYLAND (COLLEGE PARK)
KEY PROJECT "INTENSIVE SWIFT/GROUND-BASED/HST ACCRETION DISK REVERBERATION MAPPING OF THE
"BARE" ACTIVE GALACTIC NUCLEUS FAIRALL 9"
Led by Swift, Intensive Disk Reverberation Mapping (IDRM) is providing new
insights into the physics of active galactic nuclei (AGN) and strongly
challenging the standard thin accretion disk/reprocessing model of AGN
central engines. Fairall 9 is a "bare" AGN with very low absorption,
simplifying the physical interpretation. This plus the fact that it is
observable by Swift throughout the year makes it an ideal IDRM target. We
request 650 x 500 s daily visits, for which we will also obtain ground-based
ugriz at a similar cadence to measure the interband lag-wavelength relation
to perform echo mapping on the disk. We will also request HST monitoring
in year 2 of the campaign to measure the lag spectrum and disentangle
contributions to the lags from the disk and broad line region.
1417181 / PETER BROWN / TEXAS A&M UNIVERSITY
KEY PROJECT "SUPERNOVA KEY PROJECT: SWIFT RESPONSE TO NEARBY SUPERNOVAE"
Swift has proven itself to be an extraordinary supernova (SN) observatory. The clearest application of Swift’s unique strengths is obtaining very early UV and X-ray data on young SNe to constrain their progenitor systems. As part of this key project, we propose a two-year follow-up program to rapidly observe all of the nearest (distance<35 Mpc or roughly z<0.008) extragalactic transients (mostly SNe). The quick-response, distance-limited program we propose will detect any UV-bright radiative cooling following the shock breakout from core-collapse SNe and shocked companions from Type Ia SNe. Just as importantly, we will constrain the fraction of events for which it is not seen.
1417229 / THOMAS BARCLAY / UNIVERSITY OF MARYLAND (BALTIMORE COUNTY)
KEY PROJECT "A COMPREHENSIVE, MULTI-WAVELENGTH SURVEY OF COOL STAR ACTIVITY"
M-dwarfs are abundant and frequently host small planets. In the coming
decade, efforts to detect and characterize rocky planets will focus on
M-dwarfs. However, these stars are known to be highly magnetically active,
thus planets they host are subjected to significantly more radiation than
we experience from the Sun; just how much this affects their habitability
is unsettled. We propose an ambitious multi-year, multi-instrument campaign
to monitor M-dwarfs with ages from 10 Myr to 10 Gyr. X-ray, UV, and radio
observations will be combined with simultaneous high-precision optical data
from the Transiting Exoplanet Survey Satellite (TESS). The combined data
will provide a complete picture of M dwarf activity, enabling us to identify
environments conducive to harboring habitable planets.
1417232 / JAMIE KENNEA / THE PENNSYLVANIA STATE UNIVERSITY
KEY PROJECT "KEY PROJECT: THE DETECTION AND MONITORING OF ELECTROMAGNETIC COUNTERPARTS OF
GRAVITATIONAL WAVE SOURCES WITH SWIFT IN O3"
We seek to identify and follow-up EM counterparts of GW triggers detected
by ALIGO and AVirgo. To identify EM counterparts, Swift will perform a
large scale shallow tiling, covering the highest probability regions from
which the GW trigger is likely to have originated. These are selected by
convolving the GW error regions with galaxy catalogs. Based on lessons
learned during O2, including the detection of the first NS-NS merger event
with an EM counterpart, GW 170817, and through collaboration with Fermi/GBM,
we seek to improve this follow-up, maximizing the science return. In
addition we request deep follow-up observations at high priority in order
to detect and characterize any EM counterpart detected either by Swift or
other observatories, in X-ray or optical/UV.
1417018 / SYLVAIN GUIRIEC / GEORGE WASHINGTON UNIVERSITY
"TESTING A NEW MODEL FOR GRB PROMPT EMISSION FROM OPTICAL TO GAMMA-RAYS AND
EXPLORING GRBS AS STANDARD CANDLES"
The cosmological origin of Gamma Ray Bursts (GRBs) combined with their
brightness in the gamma-ray regime lead to great expectations in using
these sources as cosmological probes. In addition, the recent discovery
of gravitational waves from black hole binary mergers marks the advent
of a brand new field in astronomy in which GRBs will definitely play a
major role. However, before using GRBs as tools we must first understand
the origin and nature of the radiations released during these powerful
explosions and investigate if GRBs can be established as standard candles.
The aim of our project is to (i) probe the nature of GRB prompt emission
from optical to the gamma-rays, (ii) explore the transition between prompt
and afterglow emissions, and (iii) explore GRBs as standard candles.
1417019 / MISSAGH MEHDIPOUR / SRON NETHERLANDS INSTITUTE FOR SPACE RESEARCH
"CHASING OBSCURING WINDS WITH SWIFT"
Obscuring winds are remarkably different from the commonly seen
warm-absorber winds in AGN. They exhibit large columns of high-velocity
gas close to the black hole. They produce broad UV absorption lines and
shield much of the X-ray radiation. This has important implications for the
launching mechanism of AGN outflows. These recent extraordinary findings
were made possible by Swift monitoring of the X-ray hardness variability,
and subsequent joint observations with XMM-Newton, NuSTAR, and HST. We
propose to extend our Swift monitoring of a sample of seven suitable
AGN to broaden our understanding of this phenomenon. We request weekly
Swift monitoring of them in order to trigger joint XMM-Newton/NuSTAR/HST
ToO observations (proposed separately). In total 98 ks of Swift time is
requested.
1417037 / MARTIN HENZE / SAN DIEGO STATE UNIVERSITY
"PROBING THE ERUPTION STATISTICS AND EVOLUTION OF THE UNIQUE RECURRENT NOVA
M31N 2008-12A"
M31N 2008-12a is a recurrent nova in M31 with a unique record of 9 observed
eruptions in 9 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 2018 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.
1417043 / BERGER, EDO / HARVARD UNIVERSITY
"UNIQUE INSIGHTS INTO SWIFT GRBS WITH THE VLA AND ALMA"
Radio observations of GRB afterglows with the VLA and ALMA can address
several fundamental open questions in GRB science: (1) the composition
of the relativistic ejecta through observations of the reverse shock radio
emission, (2) the explosion properties of short GRBs, with implications for
radio counterparts of Advanced LIGO sources, and (3) whether high-redshift
GRBs form a distinct population that may point to Pop III massive star
progenitors. Here we propose to address these questions using on-going
JVLA and new ALMA programs, which represent the most comprehensive
radio/millimeter view of Swift GRBs. The proposal takes advantage of
the unparalleled sensitivity of VLA and ALMA, and builds on our long-term
success in radio studies of GRBs.
1417057 / JAKOB VAN DEN EIJNDEN / UNIVERSITEIT VAN AMSTERDAM
"THE NATURE AND ACCRETION FLOW PROPERTIES OF SUB-LUMINOUS X-RAY BINARIES"
Very-faint X-ray transients undergo outbursts of accretion with a peak
X-ray luminosity much lower than that of other black hole and neutron
star low-mass X-ray binaries. Studying these objects is of great interest
because they trace a poorly understood accretion regime and may represent a
missing population of short-period binaries or neutron stars with relatively
strong magnetic fields. To study the outburst of a very-faint X-ray
transient in detail, we propose 30 ks of Swift ToO monitoring observations
(30x1 ks every other day), and 8 hr of deep VLA radio observations (2x4 hr).
Complemented by guaranteed-time optical and near-infrared monitoring with
Faulkes and SMARTS, these data allow us to investigate the nature of the
binary and the properties of the accretion in/out flow.
1417063 / MARCO 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.
1417065 / DENNIS BODEWITS / UNIVERSITY OF MARYLAND (COLLEGE PARK)
"ROTATION AND CHEMICAL HETEROGENEITY OF HYPERACTIVE COMET 46P/WIRTANEN"
We propose to use Swift-UVOT to measure rotational variations of the gas and
dust surrounding comet 46P/Wirtanen. We will derive the rotational period
of the nucleus from continuum observations and will look for evidence of
rotational chemical variability in the production rates of OH, CN, C2, and
other volatiles. We will compare the rotation and chemical variability
before and after the comet s approach to the Sun to measure changes in the
rotation period caused by gas jets. This allows us to evaluate the chemical
heterogeneity of the nucleus, and how comets evolve through their activity.
The Swift observations will provide critical context to the anticipated
world-wide observing campaign of this close-approach comet.
1417070 / ZOLTAN HAIMAN / COLUMBIA UNIVERSITY
"TESTING THE ORIGIN OF PERIODIC VARIABILITY FOR THE BINARY CANDIDATE QUASAR
PG1302-102"
The quasar PG1302-102 exhibits periodic optical variability and was
identified as a sub-pc supermassive black hole binary (SMBHB) candidate.
If PG1302 consists of an unequal-mass SMBHB, the relativistic motion of the
secondary BH will produce strong Doppler modulations, even if the rest-frame
luminosity is constant. This effect can explain the variability in optical,
UV and X-rays (including our observations from Cycle 13). However, the
UV/X-ray light curves are sparse and, given the 5yr period of PG1302,
additional observations are needed. We propose to continue multi-wavelength
monitoring of PG1302 with UVOT and XRT to robustly test the relativistic
boost hypothesis. Swift is uniquely suited to perform this test, as it can
cover the optical, UV and X-ray bands simultaneously
1417094 / ALEXEI FILIPPENKO / UNIVERSITY OF CALIFORNIA (BERKELEY)
"GROUND-BASED OPTICAL STUDIES OF SWIFT GAMMA-RAY BURSTS, CYCLE 14"
We will continue to conduct optical photometry of Swift GRBs with the Lick
0.76-m Katzman Automatic Imaging Telescope (KAIT) to complement the optical
studies to be done with Swift (e.g., during times when the object is not
available to Swift, or more quickly and with higher cadence than Swift).
Optical photometry with the Lick Nickel 1-m telescope will be obtained
as the afterglow fades beyond KAIT’s capabilities. We will also obtain
temporal series of optical spectra, as well as deep photometry, with the
Lick 3-m and the Keck 10-m telescopes. One goal of the spectra is to search
for evidence of a supernova contribution. If circumstances permit, will
also conduct Lick/Keck spectropolarimetry of the GRB optical afterglow
and/or the supernova component, to search for asymmetries.
1417098 / OLIVIER HERVET / UNIVERSITY OF CALIFORNIA (SANTA CRUZ)
"PROBING A SCENARIO 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 VLBI
stationary 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,
particularly well adapted for the X-ray bright BL Lac Mrk 421 and the
capabilities of the Swift instruments.
1417106 / AZADEH KEIVANI / THE PENNSYLVANIA STATE UNIVERSITY
"SEEKING THE SOURCES OF THE HIGHEST-ENERGY COSMIC NEUTRINOS WITH SWIFT"
We propose further prompt searches for X-ray and UV/optical counterparts to IceCube high-energy (E>~30 TeV) likely-cosmic neutrinos with Swift. Using realtime high-energy event reconstruction algorithms running at the South Pole, we will set the selection criteria such that we will trigger four neutrinos per year. Three proposed triggers will prompt a 7-pointing mosaic by Swift, providing >50% coverage of the neutrino localization to 1 ks depth in <10 hours, while one single proposed trigger will prompt
a 19-pointing mosaic providing ~50% coverage to 1 ks depth in <16 hours. Discovery of even a single electromagnetic 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.
1417122 / ERIN KARA / UNIVERSITY OF MARYLAND (COLLEGE PARK)
"TESTING THE ULX UNIFIED MODEL WITH SWIFT MONITORING OF NGC 6946 X-1"
In recent years, a unified picture of Ultraluminous X-ray sources has
been derived from its spectral properties. In this model, the hardest,
most luminous ULXs are observed face-on, revealing the hottest part of the
super-Eddington accretion flow, while softer, less-luminous ULXs that show
evidence for Ultrafast Outflows are observed at larger inclinations. If
this unification model is correct, it should have observable implications
on the long term variability of ULXs, as the edge-on systems should show
more variability due to clumpy material along the line of sight. In this
proposal, we aim to test this model by monitoring the well-known ULX NGC
6946 X-1, which, according to the unified picture is viewed at higher
inclinations. NGC 6946 X-1 is an ideal target because, while little is
kno
1417132 / JAMIE HOLDER / UNIVERSITY OF DELAWARE
"COMPLETE PERIASTRON COVERAGE OF THE 50-YEAR BINARY PSR J2032+4127/ MT91~213."
In 2015, the gamma-ray and radio pulsar PSR~J2032+4127 was identified as
the compact object in a binary system, together with the Be star MT91
213. The source holds particular interest, as its location coincides
with a steady, extended TeV gamma-ray source, TeV J2032+4130. The binary
orbit is highly eccentric, with a period of 45-50 years and periastron
predicted for November 2017. We have been monitoring the system with Swift
throughout Cycle 13, over which time the source X-ray flux has increased
dramatically. We have established a multi-instrument observing campaign
to cover the periastron period. Here we propose continued X-ray monitoring
with Swift through Cycle 14. This will allow stringent tests of models for
the geometry and high-energy emission mechanisms in this system.
1417134 / MICHAEL SALZ / UNIVERSITAT HAMBURG
"PROBING THE MASS LOSS OF THE HOTTEST GAS PLANETS"
Close-in giant gas planets experience a continuous, photoevaporative mass
loss that can erode their gaseous envelopes. This mass loss has been
observed only in a few systems and we propose the first systematic study
in the NUV using Swift/UVOT. We proved that UVOT enables NUV photometry
better than 0.5%, sufficient for our science goals. Furthermore, our Swift
pilot study of WASP-121 showed excess NUV absorption by a thick, escaping
planetary atmosphere as predicted by our simulations; a feature previously
only known for WASP-12 b and HD 209458b. We now propose to measure the NUV
transit depth of six carefully selected hot gas giant planets to measure
their NUV transit depth. This allows us to test models, which make clear
predictions for the NUV absorption depending on irradiation level.
1417137 / JAMES NEILL / CALIFORNIA INSTITUTE OF TECHNOLOGY
"ROBOTIC SPECTROSCOPIC FOLLOWUP OF SWIFT GRBS"
We propose rapid and robotic multicolor imaging and spectroscopy of
GRB afterglows on the Palomar 60-inch telescope. Robotic spectroscopy
is available on the fully proven Spectral Energy Distribution Machine
(a low resolution integral field spectrograph). Our annual yield is
expected to be ten multi-band photometric observations and five redshifts.
We will disseminate these findings quickly and thereby enable wider
follow up of SWIFT bursts. The goals of our group are are: (i) provide
automated, rapid spectroscopy enabling immediate redshift measurement and
sensitive constraints on the color evolution of GRBs; (ii) rapidly identify
high-redshift and dust-obscured GRBs; (iii) identify reverse shocks and
constrain energetics of GRBs; (iv) collect unbiased samples for demographic
study.
1417138 / RAFFAELLA MARGUTTI / 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 circum stellar medium interaction.
1417139 / EDWARD CACKETT / WAYNE STATE UNIVERSITY
"ACCRETION DISK REVERBERATION MAPPING OF A SUPER-EDDINGTON AGN"
At high mass accretion rates, accretion disks are expected to be
significantly different from the standard optically thick, geometrically
thin disk. However, observational tests of disk structure are rare.
Emission line reverberation mapping has revealed that the broad line
region in super-Eddington AGN are quite different, but what about the
disk? The accretion disk reverberation mapping technique provides a
way to observationally test the structure of the accretion disk at high
accretion rates. Through flexible and high-cadence monitoring, Swift has
revolutionized accretion disk reverberation over the last few years. Here,
we propose to apply this technique to a super-Eddington AGN for the first
time, to explore the structure of disks at extreme mass accretion rates.
1417151 / ANDREAS ZEZAS / HARVARD-SMITHSONIAN CENTER FOR ASTROPHYSICS
"REVEALING THE TRANSIENT X-RAY BINARY POPULATION OF THE LMC"
We propose systematic monitoring observations of 25 fields in the Large
Magellanic Cloud (LMC) with quasi-bi-weekly cadence. This will be the first
dedicated X-ray monitoring campaign of a large area of the LMC. With these
observations we will: (a) identify the elusive, transient High-Mass X-ray
binary (HMXB) populations in the LMC; (b) obtain a more complete census of
its HMXB populations that will allow us to better constrain their formation
efficiency; (c) constrain their orbital periods; (d) identify new accreting
pulsars. Through this campaign we will study the populations of HMXBs in a
galaxy with a metallicity bridging the gap between the SMC and our Galaxy,
allowing us to constrain models for their formation and evolution.
1417156 / DHEERAJ PASHAM / MASSACHUSETTS INSTITUTE OF TECHNOLOGY
"XRT AND UVOT MONITORING OF THE TIDAL DISRUPTION FLARE ASASSN-14LI TO DETECT
THE NEWLY FORMED ACCRETION DISK"
We propose high-cadence XRT and UVOT monitoring observations (2ksx8
visits per day for 3 days) of Rosetta Stone tidal disruption flare (TDF)
ASASSN-14li at late times. Our main goals are (1) search for a correlation
between the X-ray and UV light curves, and (2) detect an X-ray-UV time
lag/lead in the range of a few hours to tens of hours. Any detected lag
will not only establish unambiguously the presence of an accretion disk in
a TDF for the first time, but will also directly give us the minimum size
of the putative disk. ASASSN-14li is currently the only TDF where such
measurements can be made. Swift, with its excellent X-ray sensitivity and
UV capability, combined with fast maneuvering ability, is currently the only
observatory that can perform simultaneous X-ray and UV observations.
1417159 / MARIANNE VESTERGAARD / UNIVERSITY OF ARIZONA
"TOO MONITORING OF THE RE-AWAKENING AGN IN MRK590: CATCHING THE MONSTER IN THEACT!"
After a 10-year hiatus, Mrk590 appears to be rekindling its nuclear
activity! Existing Swift data strongly suggest that the AGN is likely to
turn on again in the near future. We wish to seize this rare and fortuitous
opportunity to document, for the first time ever, the onset of AGN activity
since this can lead to significant insight on the long-standing issue of
how AGNs are fueled. Once triggered by another program (PI:Vestergaard)
we ask to first observe Mrk590 ~daily with Swift for up to 60 days and then
for 5 ~bi-weekly follow-up observations to establish if Mrk590 has entered a
stable high or low flux state. We also ask for two 20ks NuSTAR observations
to place tighter constraints on the potential emergence of a weak soft X-ray
component and perhaps a high-energy reflection component
"MONITORING THE SLEEPING MONSTER IN AGN MRK590 AND CLUES TO THE NATURE OF ITS
RADIO EMISSION"
After a 10-year hiatus, Mrk590 appears to be rekindling its nuclear
activity! Existing Swift data strongly suggest that the AGN is likely to
turn on again in the near future. We wish to seize this rare and fortuitous
opportunity to document, for the first time ever, the onset of AGN activity
as it occurs since this can lead to significant insight on the long-standing
problem of how AGNs are fuelled. We propose to monitor Mrk590 with Swift
(biweekly) and with the VLBA (~bi-monthly). We aim to determine the nature
of the radio emission, confirm its connection to the X-ray processes, and to
record the potential black hole state changes from low/hard to high/soft
states that have not yet been observed for massive black holes. This
program is a trigger for another program (PI: Vestergaard).
1417179 / FELIX FUERST / EUROPEAN SPACE ASTRONOMY CENTRE (ESAC)
"SWIFT MONITORING OF NEUTRON STAR POWERED ULTRA-LUMINOUS X-RAY SOURCES"
Following a series of remarkable recent discoveries, we now know that
some of the most luminous members of the ultraluminous X-ray source (ULX)
population are actually powered by highly super-Eddington neutron star
accretors. Three such systems are known: M82 X-2, NGC 7793 P13, and
NGC 5907 ULX1. Here we propose to extend our successful Swift monitoring
program performed in the last AOs of the latter two of these systems. NGC
7793 P13 and NGC 5907 ULX1 are sufficiently isolated for Swift to provide
robust fluxes, across the full visibility window available for each source
in the upcoming cycle. These observations will help to reveal the nature
and physical properties of the most extreme accretors known.
1417202 / LEA HAGEN / SPACE TELESCOPE SCIENCE INSTITUTE
"MODELING THE PHYSICAL PARAMETERS AND ULTRAVIOLET DUST EXTINCTION CURVE IN FIVE
NEARBY DWARF GALAXIES"
We propose to use Swift/UVOT to observe five recently-discovered dwarf
galaxies in the Local Volume. We will combine new observations in the
UV filters with archival optical imaging to model the spectral energy
distributions (SEDs) of each tiny galaxy, revealing information including
the shape of the dust extinction curve, stellar masses, and star formation
history. This information will contribute to our understanding of the
formation and evolution of dwarf galaxies, which in turn will inform
theories for the growth of structure at small scales.
1417210 / JEROEN HOMAN / EUREKA SCIENTIFIC INC.
"A RARE LOOK AT A BLACK HOLE TRANSIENT EMERGING FROM QUIESCENCE"
Given the limited sensitivity of all-sky-monitors and the unpredictability
of black hole transients, the early phases of their outbursts are typically
not well covered. We propose a brief and well-timed Swift monitoring
campaign to catch the rise of the next outburst of the black hole transient
H1743-322. The regularity of its outbursts (once every ~245-270 days)
provides us with a rare opportunity to follow a transient as it emerges from
quiescence. Our X-ray observations will complement near-IR monitoring and
we request additional VLA observations during the outburst rise. The goals
of this campaign are to provide input to outburst disk-instability models
and to study disk-jet coupling during outburst rise. We request a maximum
of 43 (1 ks) Swift observations and 5 hrs of VLA time.
1417036 / STEFANO MARCHESI / CLEMSON UNIVERSITY
"THE LEGACY OF SWIFT-BAT: THE TALE OF AGN AT HARD X-RAYS"
We propose a quick snapshot program with Swift to observe the remaining 29 AGN detected in the 100 month BAT survey that do not have any X-ray observation in the 0.5-10 keV band. These AGN are expected to be mostly absorbed by LogNH<23 and as such are the perfect targets for a 5ks observation (each) with Swift. This will render complete the 100m high-latitude BAT survey, providing a heritage-quality sample that we will use to: 1) address the space density of Compton-thick AGN, 2) verify whether absorbed AGN are intrinsically less luminous than unabsorbed one, and 3) study the evolution of the most powerful blazars.
- Curator: J.D. Myers
- NASA Official & Swift PI: Brad Cenko
- PAO Contact: Francis Reddy
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