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J/A+A/610/A14       ASASSN-15lh MUSE host spectroscopy         (Kruehler+, 2018)

The supermassive black hole coincident with the luminous transient ASASSN-15lh Kruehler T., Fraser M., Leloudas G., Schulze S., Stone N.C., van Velzen S., Amorin R., Hjorth J., Jonker P.G., Kann D.A., Kim S., Kuncarayakti H., Mehner A., Nicuesa Guelbenzu A. <Astron. Astrophys. 610, A14 (2018)> =2018A&A...610A..14K (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Supernovae Keywords: stars: individual: ASASSN-15lh - galaxies: supermassive black holes Abstract: The progenitors of astronomical transients are linked to a specific stellar population and galactic environment, and observing their host galaxies hence constrains the physical nature of the transient itself. Here, we use imaging from the Hubble Space Telescope, and spatially resolved, medium-resolution spectroscopy from the Very Large Telescope obtained with X-shooter and MUSE to study the host of the very luminous transient ASASSN-15lh. The dominant stellar population at the transient site is old (around 1 to 2Gyr) without signs of recent star formation. We also detect emission from ionized gas, originating from three different, time invariable, narrow components of collisionally excited metal and Balmer lines. The ratios of emission lines in the Baldwin-Phillips-Terlevich diagnostic diagram indicate that the ionization source is a weak active galactic nucleus with a black hole mass of MBH=5-3+8x108M, derived through the M*-σ relation. The narrow line components show spatial and velocity offsets on scales of 1kpc and 500km/s, respectively; these offsets are best explained by gas kinematics in the narrow-line region. The location of the central component, which we argue is also the position of the supermassive black hole, aligns with that of the transient within an uncertainty of 170pc. Using this positional coincidence as well as other similarities with the hosts of tidal disruption events, we strengthen the argument that the transient emission observed as ASASSN-15lh is related to the disruption of a star around a supermassive black hole, most probably spinning with a Kerr parameter aBH≥0.5. Description: The two data files with fits extension (ASASSN-15lhastphotcube_2016.fits and ASASSN-15lhastphotcube_2017.fits) are three-dimensional fits files with a primary header and two extensions: The primary header contains only the fits headers. The first fits extensions (DATA) contain the observed flux values in units of 10E-20erg/cm2/s/Å. The dimensions of the cubes are 330x325x3681 for the 2016 data, and 317x323x3681 for the 2017 data, respectively. The first two dimensions are celestial coordinates (RA, DEC), and the last one the wavelength coordinate in Angstrom. The second fits extensions (STAT) contain the estimated variance in units of 10E-40erg-2cm-4s-2Å-2. Objects: ------------------------------------------------------- RA (2000) DE Designation(s) ------------------------------------------------------- 22 02 15.45 -61 39 34.6 ASASSN -15lh = SN 2015L ------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 129 2 List of fits datacubes fits/* 0 2 Individual datacubes
See also: J/ApJ/828/3 : Swift obs. of the superluminous SNI ASASSN-15lh (Brown+, 2016) Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000) 10- 18 F9.5 deg DEdeg Declination of center (J2000) 20- 22 F3.1 arcsec/pix scale Scale of the image 24- 26 I3 --- Nx Number of pixels along X-axis 28- 30 I3 --- Ny Number of pixels along Y-axis 32- 35 I4 --- Nz Number of slices 37- 43 I7 Kibyte size Size of FITS file 45- 78 A34 --- FileName Name of FITS file, in subdirectory fits 80-129 A50 --- Title Title of the FITS file
Acknowledgements: Thomas Kruehler, t.kruehler(at)
(End) Patricia Vannier [CDS] 30-Oct-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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