AT 2019avd
RA/DEC (2000)
08:23:36.767 +04:23:02.46
125.9031975 +4.3840166
Type
AGN
Redshift
0.028
Related AstroNotes: 2020-105
Reporting Group
ZTF
Discovering Data Source
ZTF
Discovery Date
2019-02-09 05:28:19.000
TNS AT
Y
Public
Y
Discovery Mag
17.45
Filter
r-ZTF
Reporter/s
J. Nordin, V. Brinnel, M. Giomi, J. van Santen (HU Berlin), A. Gal-Yam, O. Yaron, S. Schulze (Weizmann) on behalf of ZTF

Spectra

 AT_2019avd - 2020-05-10 08:18:34 FTS / FLOYDS-S (None)z=
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   Binning factor: (rounded to nearest integer >1)
Mouse hovers at WL: 0 (rest),0 (observed)
Spectra
SelectIDObs-date (UT)Tel / InstExp-TimeObserver/sReducer/sGroupSpectrum ascii fileSpectrum fits fileSpec. TypeAssoc. GroupsEnd prop. periodRemarks
66452020-05-10 08:18:34FTS / FLOYDS-S3600Las Cumbres ObservatoryJamie BurkeNone tns_2019avd_2020-05-10_08-18-34_FTS_FLOYDS-S.ascii tns_2019avd_2020-05-10_08-18-34_FTS_FLOYDS-S.fitsObjectNo standard star taken this night. Peak of Balmer lines indicates z=0.028 or 0.0285 (Hbeta or Halpha, respectively).
Light Curves
FilterTel / InstObs-date rangePhotometry
orange-ATLASATLAS1_ACAM12020-04-25 06:44:38 - 2020-04-27 06:01:262
Photometry
IDObs-dateMag. / FluxErrLim. Mag./FluxUnitsFilterTel / InstExp-timeObserver/sRemarks
1373092020-04-27 06:01:2618.8470.15819.47ABMagorange-ATLASATLAS1_ACAM130Robot
1373082020-04-25 06:44:3819.24ABMagorange-ATLASATLAS1_ACAM130Robot[Last non detection]
r-ZTFP48_ZTF-Cam2019-01-26 06:56:26 - 2019-02-12 05:26:053
Photometry
IDObs-dateMag. / FluxErrLim. Mag./FluxUnitsFilterTel / InstExp-timeObserver/sRemarks
536522019-02-12 05:26:0517.450.0420.18ABMagr-ZTFP48_ZTF-Cam30
536532019-02-09 05:28:1917.640.0720.34ABMagr-ZTFP48_ZTF-Cam30
536512019-01-26 06:56:2619.66ABMagr-ZTFP48_ZTF-Cam30[Last non detection]
AT Reports
IDTime received (UT)SenderReporter/sReportting groupDisc. Data SourceRADECDiscovery date (UT)Discovery Mag.FilterRelated filesAT TypeInternal nameAssoc. GroupsEnd prop. periodRemarks
710412020-05-17 14:48:29ATLAS_Bot1J. Tonry, L. Denneau, A. Heinze, H. Weiland, H. Flewelling (IfA, University of Hawaii), B. Stalder (LSST), A. Rest (STScI), C. Stubbs (Harvard University), K. W. Smith, S. J. Smartt, D. R. Young, S. Srivastav, O. McBrien, D. O'Neill, P. Clark, M. Fulton, J. Gillanders, M. Dobson (Queen's University Belfast), T.-W. Chen (MPE), D. E. Wright (University of Minnesota), J. Anderson (ESO)ATLASATLAS08:23:36.844+04:23:02.022020-04-27 06:01:26.40018.847orange-ATLASPSNATLAS19bfsoATLAS
299102019-02-12 13:55:54ZTF_AMPEL_NEWJ. Nordin, V. Brinnel, M. Giomi, J. van Santen (HU Berlin), A. Gal-Yam, O. Yaron, S. Schulze (Weizmann) on behalf of ZTFZTFZTF08:23:36.767+04:23:02.462019-02-09 05:28:19.00017.45r-ZTFPSNZTF19aaiqmglZTF
Classification Reports
IDTime received (UT)SenderClassifier/sGroupClassificationRedshiftRelated filesAssoc. GroupsEnd prop. periodRemarksADS Bibcode
66342020-05-17 14:14:51benny.trakhtBenny Trakhtenbrot (TAU), Iair Arcavi (TAU), Claudio Ricci (UDP), Jamie Burke (UCSB/LCO)NoneAGN0.028AT 2019avd (also known as ZTF19aaiqmgl) was originally identified as an optical transient in the nucleus of a galaxy at z=0.0296, by the ZTF, on 2019 Feb. 9. After about 10 months of decline, it had another, slower re-brightening, reaching a secondary peak during April 2020. On April 28, eROSITA detected a new, ultra-soft X-ray source associated with the galaxy nucleus (ATel #13712), with a factor 90x (at least) increase in X-ray emission, compared to an XMM upper-limit from 2015. We obtained an optical spectrum of AT 2019avd using the Las Cumbres Observatory 2m telescope at Siding Spring (Australia) during the night of 2020 May 10. The spectrum, publicly available on the TNS, shows a combination of AGN-like emission lines (specifically, NLSy1-like Halpha) as well as a very strong, broad and double-peaked emission feature around 4680A (rest-frame), consistent with the expected location of the HeII4686 and NII4640 emission lines. These features are much stronger than seen in AGN, with F(NIII)~F(HeII) > 0.5*F(Hbeta), and are likely driven by intense UV flares which excite the relevant Bowen fluorescence (BF) cascades. Our new optical spectrum of AT 2019avd therefore shares the key characteristics of the recently identified class of transients from accreting SMBHs, with the best-studied example being AT 2017bgt (Trakhtenbrot et al. 2019, Nature Astronomy, 3, 242). We note that Gezari et al. (ATel #13717) report that an earlier spectrum of AT 2019avd, obtained on 2019 Mar 15, shows no such BF features. Since similar (transient) BF features have also been reported in a number TDE candidates (Leloudas+19, ApJ 887, 218; Gezari+19, ATel #13127) and other nuclear transients (Neustadt+20, MNRAS 494, 2538), the nature of AT 2019avd remains unclear. We are pursuing additional spectreoscopic and multi-wavelength observations of AT 2019avd. 2020TNSCR1391....1T