VizieR Online Data Catalog: UV and optical LCs of the TDE AT2021ehb (Yao+, 2022)

In this paper, we present an in-depth study of the X-ray, UV, optical, and radio emission of AT2021ehb, using observations obtained from 2021 March 1 to 2022 May 31.

We obtained ZTF mosaic camera forced photometry on the Palomar Oschin Schmidt 48 inch (P48) telescope in the g and the r bands using the median position of all ZTF alerts up to MJD59550 (RAJ200=03:07:47.82,DEJ2000=40:18:40.85). See Section 2.1.1

We obtained additional ugri photometry using the Spectral Energy Distribution Machine (SEDM) on the robotic Palomar 60 inch telescope (P60), and the optical imager on the Liverpool Telescope (LT). See Section 2.2.

We obtained low-resolution optical spectroscopic observations using the Low Resolution Imaging Spectrograph (LRIS) on the Keck I telescope, the Double Spectrograph (DBSP) on the 200 inch Hale telescope, the integral field unit (R~100) spectrograph of SEDM, and the De Veny Spectrograph on the Lowell Discovery Telescope (LDT). We also obtained a medium-resolution spectrum using the Echellette Spectrograph and Imager (ESI) on the Keck II telescope. See Section 2.3.

AT2021ehb was observed by the X-Ray Telescope (XRT) and the Ultra-Violet/Optical Telescope (UVOT) on board Swift under our GO program 1619088 (as ZTF21aanxhjv; target ID 14217; PI: Gezari) and a series of time-of-opportunity (ToO) requests (PI: Yao). The first four UVOT epochs (obsID 14217001-14217005) were conducted with UBV+All UV filters. Subsequent observations were conducted with U+All UV filters. See Section 2.4.

AT2021ehb was observed by NICER under Director's Discretionary Time (DDT) programs on 2021 March 26, 2021 Jul 2-7, and from 2021 Nov 13 to 2022 Mar 29 (PIs: Yao, Gendreau, Pasham). See Section 2.5.

We obtained two epochs of follow-up observations with XMM-Newton/EPIC under our Announcement of Opportunity program (PI: Gezari), on 2021 Aug 4 (obsID 0882590101) and 2022 Jan 25 (obsID 0882590901). See Section 2.6.

The location of AT2021ehb was scanned by eROSITA as part of the planned eight all-sky surveys. See Section 2.7.

We obtained NuSTAR observations under a preapproved ToO program (PI: Yao; obsID 80701509002) and a DDT program (PI: Yao; obsID 90801501002). The first epoch was conducted from 2021 Nov 18.8 to 19.9 with an exposure time of 43.2ks. The second epoch was conducted from 2022 Jan 10.4 to 12.1 with an exposure time of 77.5ks. See Section 2.8

We began a monitoring program of AT2021ehb using the Very Large Array (VLA) under program 20B-377 (PI Alexander). AT2021ehb was not detected in any of our observations. See Section 2.9.

(1 data file).