VizieR Online Data Catalog: 500days of ASASSN-18pg multiwavelength obs. (Holoien+, 2020)
Abstract
The All-Sky Automated Survey for Supernovae (ASAS-SN; Shappee+ 2014, J/ApJ/788/48) currently is composed of five units hosted by the Las Cumbres Observatory global telescope network in Hawaii, Chile, Texas, and South Africa. To construct the V-band reference image, we used only data obtained prior to 2018 May 1, and for the g-band reference image, we used only data obtained after 2019 April 1. See Section 2.2.
Our initial Swift follow-up campaign included 25 epochs of TOO observations between 2018 July 18 and 2018 November 6. We obtained an additional 28 epochs of observations between 2019 January 22 and 2019 October 29. UVOT observations were obtained in the V (5468Å), B (4392Å), U (3465Å), UVW1 (2600Å), UVM2 (2246Å), and UVW2 (1928Å) filters in most epochs. See Section 2.3. We also obtained uBVgri observations from the Swope 1m telescope at Las Campanas Observatory and BVgri observations from the Las Cumbres Observatory 0.4 and 1m telescopes located in Cerro Tololo, Chile; Siding Spring, Australia; and Sutherland, South Africa. See Section 2.4. We began spectroscopic follow-up observations of ASASSN-18pg following its classification as a possible TDE and continued to monitor it regularly through 2019 September. Our follow-up spectra were obtained with the Robert Stobie Spectrograph (RSS) on the 10m SALT, the Gemini Multi-Object Spectrograph (GMOS) on the 8.4m Gemini South telescope, the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan-Baade telescope, LDSS-3 on the 6.5m Magellan Clay telescope, the Goodman Spectrograph on the Southern Astrophysical Research (SOAR) 4.1m telescope, and the Wide Field Reimaging CCD Camera (WFCCD) on the du Pont 100 inch telescope. Our observations span from 26 days prior to peak light through 272 days after and include several spectra taken near or before peak light. See Section 2.5. We observed ASASSN-18pg using the Australia Telescope Compact Array (ATCA) in the 15mm band, using the Compact Array Broadband Backend to provide 2x2048MHz of bandwidth, centered at 16.7 and 21.2GHz. Our initial observation was made on 2018 July 20 (08:18-13:29 UT). We made a second ATCA observation on 2018 August 6 (12:20-17:18 UT). We conclude that ASASSN-18pg was not detected in the radio. We note, however, that both of these observations were taken prior to ASASSN-18pg reaching its peak brightness (see Section 3.1), so it is possible that the tidal disruption event (TDE) could have exhibited radio emission at later times that was not detectable prior to peak. See Section 2.6. (2 data files).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- November 2021
- DOI:
- 10.26093/cds/vizier.18980161
- Bibcode:
- 2021yCat..18980161H
- Keywords:
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- Photometry: ultraviolet;
- Photometry: UBVRI;
- Spectra: optical