VizieR Online Data Catalog: Photometry of the tidal disruption event PS18kh (Holoien+, 2019)
Abstract
We retrieved archival optical ugriz model magnitudes of SDSS J075654.53+341543.6 from SDSS Data Release 14 (DR14; Abolfathi+ 2018ApJS..235...42A) and infrared W1 and W2 magnitudes from the Wide-field Infrared Survey Explorer (WISE) AllWISE catalog (II/328). The host is not detected in archival data from, or was not previously observed by, the Two Micron All-sky Survey, Spitzer, Herschel, the Hubble Space Telescope, the Chandra X-ray Observatory, the X-ray Multi-mirror Mission, or the Very Large Array Faint Images of the Radio Sky at Twenty-cm survey. It is also not detected in Galaxy Evolution Explorer (GALEX) UV data, but we obtain 3σ 6.0" upper limits on the UV magnitudes of NUV>23.65 and FUV>23.69 using single-epoch data obtained on 2008 January 19. See Section 2.1.
The Pan-STARRS1 griz photometry, ASAS-SN photometric measurements, and ATLAS o-band photometry are presented in Table 3. The Pan-STARRS1 telescope, located at the summit of Haleakala on Maui, has a 1.8m diameter primary mirror. See Section 2.2. The All-sky Automated Survey for Supernovae (ASAS-SN; Shappee+ 2014ApJ...788...48S) uses units of four 14cm telescopes on a common mount located at multiple sites in both hemispheres and hosted by the Las Cumbres Observatory global telescope network. See Section 2.3. The Asteroid Terrestrial-impact Last Alert System (ATLAS; Tonry+ 2018PASP..130f4505T) uses fully robotic 0.5m f/2 Wright Schmidt telescopes located on the summit of Haleakala and at Mauna Loa Observatory to monitor the entire sky visible from Hawaii every few days. See Section 2.4. After PS18kh was classified as a tidal disruption event (TDE) candidate, we were awarded 20 epochs of Swift TOO observations of PS18kh between 2018 March 27 and 2018 May 29, after which it became Sun-constrained. The UVOT observations were obtained in the V (5468Å), B (4392Å), U (3465Å), UVW1 (2600Å), UVM2 (2246Å), and UVW2 (1928Å) filters for all epochs. See Section 2.5. In addition to the survey data and Swift observations, we obtained photometric observations from multiple ground observatories. BVgri observations were obtained from the 2m Liverpool Telescope (LT) and from the 24 inch Post Observatory (PO) robotic telescopes located in Mayhill, New Mexico, and Sierra Remote Observatory in California. Additional u-band data were obtained with MegaCam on the CFHT. See Section 2.6. After classifying PS18kh as a TDE candidate, we began a program of spectroscopic follow-up to complement our photometric follow-up. The telescopes and instruments used to obtain follow-up spectra as part of this campaign included SNIFS on the University of Hawaii 88 inch telescope, the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan-Baade telescope, the Gemini Multi-Object Spectrograph (GMOS) on the 8.2m Gemini North telescope, the SPectrograph for the Rapid Acquisition of Transients (SPRAT) on the Liverpool Telescope, the Low-Resolution Imaging Spectrometer (LRIS) on the Keck I 10m telescope, and the Multi-Object Double Spectrographs MODS) mounted on the dual 8.4m Large Binocular Telescope (LBT). See Section 2.7. (1 data file).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- January 2021
- DOI:
- 10.26093/cds/vizier.18800120
- Bibcode:
- 2021yCat..18800120H
- Keywords:
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- Photometry: ultraviolet;
- Photometry: ugriz