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Characterizing some Gaia Alerts with LAMOST and SDSS

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Abstract

The ESA-Gaia satellite is regularly producing Alerts on objects where photometric variability has been detected after several passages over the same region of the sky. The physical nature of these objects has often to be determined with the help of complementary observations from ground-based facilities. We have compared the list of Gaia Alerts (from the beginning in 2014 to Nov. 1st, 2018) with archival LAMOST and SDSS spectroscopic data. A search radius of 3″ has been adopted. In using survey data, the date of the ground-based observation rarely corresponds to the date of the Alert, but this allows at least the identification of the source if it is persistent, or the host galaxy if the object was only transient like a supernova (SN). Some of the objects have several LAMOST observations, and we complemented this search by adding also SDSS DR15 data in order to look for long-term variability. A list of Gaia Nuclear Transients (GNT) from Kostrzewa-Rutkowska et al. (Mon. Not. R. Astron. Soc. 481(1):307, 2018) has been included in this search also. We found 26 Gaia Alerts with spectra in LAMOST+SDSS labelled as stars, among which 12 have multi-epoch spectra. A majority of them are Cataclysmic Variables (CVs). Similarly, 206 Gaia Alerts have associated spectra labelled as galaxies, among which 49 have multi-epoch spectra. Those spectra were generally obtained on a date widely different from the Alert date, and are mostly emission-line galaxies with no particularity (except a few Seyferts), leading to the suspicion that most of the Alerts were due to a SN. As for the GNT list, we found 55 associated spectra labelled as galaxies, among them 13 with multi-epoch spectra. In these two galaxy samples, in only two cases, Gaia17aal and GNTJ170213+2543, was the date of the spectroscopic observation close enough to the Alert date: we find a trace of the SN itself in their LAMOST spectrum, both being now classified here as a type Ia SN. Compared to the galaxy sample from the Gaia alerts, the GNT sample has a higher proportion of AGNs, suggesting that some of the detected variations are also due to the AGN itself. Similarly for Quasars, we found only 30 Gaia Alerts but 68 GNT cases associated with single epoch quasar spectra in the databases. In addition to those, 12 plus 23 are quasars where multi-epoch spectra are available. For ten out of these 35, their multi-epoch spectra show appearance or disappearance of the broad Balmer lines and also variations in the continuum, qualifying them as “Changing Look Quasars” and therefore significantly increasing the available sample of such objects.

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Notes

  1. http://gsaweb.ast.cam.ac.uk/alerts.

  2. http://dr5.lamost.org.

  3. http://ooruri.kusastro.kyoto-u.ac.jp/mailarchive/vsnet-alert/1231.

  4. Note that although the initial GNT sample comprises 482 targets selected as having a SDSS counterpart, only about one third of them have a SDSS spectrum for classification, the rest of the sample having only SDSS photometry.

  5. These are Gaia17aqc, a blue source with previous variability in CSS, too faint for LAMOST, with a photometric redshift of 0.925; Gaia17bmd, a UV and radio source with no measured redshift, but a single epoch LAMOST spectrum shows a single emission line giving z = 0.159 if identified to H\(\alpha \), to be confirmed; Gaia17cdu, a candidate SN in a LEDA galaxy with cz = 31028 km/s, alerted at g = 18.9, giving an absolute magnitude of −19.3, compatible with a type Ia SN; and GNT J000121-0011, a NED galaxy with z = 0.462, but no identifiable features in the SDSS spectrum.

  6. They probably also correspond to a unique Gaia target, but detected at different scanning angles, not recognized as such in the very early phase of the survey.

  7. The SDSS class QSO comprises two subclasses, either “Broadline”, or “Starburst/Broadline”, the latter corresponding more to lower luminosity objects where the broadline component is not dominant.

  8. Note that this object is the only one in common with their sample.

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Acknowledgements

This work was initiated during a visit to SWIFAR (in the frame of the Chinese-French LIA “Origins” program), whose hospitality and support are gratefully acknowledged by MD. ZYH thanks Dr. Wei Zhang, Zhongrui Bai and Dongwei Fan for helpful discussions. ZYH and XWL have been partially supported by the National Key Basic Research Program of China 2014CB845700. TMZ is supported by the NSFC 11633002. We acknowledge the use of data from the ESA Gaia Satellite, DPAC and the Photometric Science Alerts Team (http://gsaweb.ast.cam.ac.uk/alerts).

The Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences.

We used data from the Sloan Digital Sky Survey (SDSS) public releases. Funding for the SDSS has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions (details on the SDSS web site at www.sdss.org).

This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology.

We thank an anonymous referee for valuable comments which helped to improve the manuscript.

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Authors and Affiliations

  1. Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 10101, Beijing, P.R. China

    Z. Huo & T. Zhang

  2. Institute of Astrophysics Paris (IAP), and Sorbonne University, 98bis Boulevard Arago, 75014, Paris, France

    M. Dennefeld

  3. South-Western Institute For Astronomy Research (SWIFAR), Yunnan University, Kunming, Yunnan, 650091, P.R. China

    X. Liu

  4. Nordic Optical Telescope (NOT), Apartado 474, 38700, Santa Cruz de La Palma, Spain

    T. Pursimo

  5. School of Astronomy and Space Science, University of Chinese Academy of Sciences, 101408, Beijing, P.R. China

    T. Zhang

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  1. Z. Huo
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  2. M. Dennefeld
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  3. X. Liu
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Appendix A: Tables

Appendix A: Tables

Spectral information for the Gaia Alerts and the GNT sample are given in the Tables below. Here we only display a few lines as examples, while the full Tables are available on line only. Table A.1 lists all the 387 spectral information available for the 285 targets in the Gaia Alerts. This includes the name of the object, Ra and Dec in decimal degrees, the mean historic magnitude in the Gaia G band, the G band magnitude at the time of the alert, the date of the alert, the date of the spectral observation, the origin of the spectra (LAMOST or SDSS), Ra and Dec of the spectral data in decimal degrees, redshift, class and subclass of the object, the spectral type of the object: emission or absorption line star/galaxy (star: ELS/ALS, galaxy: ELG/ALG; if both emission and absorption lines are present, we note E+A or A+E), and comments about the origin of the photometric variability, if available.

Table A.1 Spectral information for Gaia alert targets
Full size table

Table A.2 lists all the 192 spectral information for the 146 targets in the GNT list, the columns are the same as in Table A.1, except that the name, the G band medium magnitude, the G band peak magnitude, and the date of the G band peak are taken from Kostrzewa-Rutkowska et al. (2018). Some additions/corrections are introduced in this table since their work, also a few more identifications and redshifts (from LAMOST, SDSS or NOT) as indicated in the comments, and the multi-spectra description. Full tables will be available at CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/other/A+SP.

Table A.2 Spectral information for GNT targets
Full size table

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Huo, Z., Dennefeld, M., Liu, X. et al. Characterizing some Gaia Alerts with LAMOST and SDSS. Astrophys Space Sci 365, 89 (2020). https://doi.org/10.1007/s10509-020-03804-7

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