J/A+A/602/A28 IR signature of CMBH in nearby dwarf galaxies (Marleau+, 2017)
Infrared signature of active massive black holes in nearby dwarf galaxies.
Marleau F.R., Clancy D., Habas R., Bianconi M.
<Astron. Astrophys. 602, A28 (2017)>
=2017A&A...602A..28M 2017A&A...602A..28M (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Galaxies, IR ; Redshifts
Keywords: galaxies: general - galaxies: Seyfert - galaxies: active -
galaxies: dwarfs - Local Group - infrared: galaxies
Abstract:
We investigate the possible presence of active galactic nuclei (AGN)
in dwarf galaxies and other nearby galaxies to identify candidates for
follow-up confirmation and dynamical mass measurements.
We identify candidate active central massive black holes (CMBH) using
their mid-infrared emission, verify their nature using existing
catalogues and optical line emission diagnostics, and study the
relationship between their mass and the mass of their host galaxy.
We use the Wide-field Infrared Survey Explorer (WISE) All-Sky Release
Source Catalog and examine the infrared colours of a sample of dwarf
galaxies and other nearby galaxies in order to identify both
unobscured and obscured candidate AGN by applying the infrared colour
diagnostic. Stellar masses of galaxies are obtained using a
combination of three independent methods. Black hole masses are
estimated using the bolometric luminosity of the AGN candidates and
computed for three cases of the bolometric-to-Eddington luminosity
ratio.
We identify 303 candidate AGN, of which 276 were subsequently found to
have been independently identified as AGN via other methods. The
remaining 9% require follow-up observations for confirmation. The
activity is detected in galaxies with stellar masses from ∼106 to
109M☉; assuming the candidates are AGN, the black hole masses
are estimated to be ∼103-106M☉, adopting Lbol=0.1LEdd.
The black hole masses probed are several orders of magnitude smaller
than previously reported for centrally located massive black holes. We
examine the stellar mass versus black hole mass relationship in this
low galaxy mass regime. We find that it is consistent with the
existing relation extending linearly (in log-log space) into the lower
mass regime.
These findings suggest that CMBH are present in low-mass galaxies and
in the Local Universe, and provide new impetus for follow-up dynamical
studies of quiescent black holes in local dwarf galaxies.
Description:
List of dwarf (table2.dat) and non-dwarf (table3.dat) galaxies with IR
signatures of active massive black holes. The entries in each table
include: name, right ascension and declination (J2000), redshift,
distance in Mpc, log of stellar mass measured from SED fit, WISE
colours, log of central black hole mass estimates based on IR
luminosity (assuming Lbol=0.1LEdd), and image number in Figure 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 102 62 List of dwarf galaxies with IR signatures of
active massive black holes
table3.dat 102 241 List of non-dwarf galaxies with IR signatures of
active massive black holes
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See also:
J/ApJ/670/92 : New sample of low-mass black holes in AGN (Greene+, 2007)
J/ApJ/755/167 : Low-mass black holes in SDSS Seyfert 1 galaxies (Dong+, 2012)
J/ApJ/775/116 : z<0.06 active black hole galaxies from SDSS-DR8 (Reines+, 2013)
Byte-by-byte Description of file: table2.dat table3.dat
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Bytes Format Units Label Explanations
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1- 28 A28 --- Name Name
29- 30 I2 h RAh Source right ascension (J2000)
32- 33 I2 min RAm Source right ascension (J2000)
35- 39 F5.2 s RAs Source right ascension (J2000)
41 A1 --- DE- Source declination sign (J2000)
42- 43 I2 deg DEd Source declination (J2000)
45- 46 I2 arcmin DEm Source declination (J2000)
48- 51 F4.1 arcsec DEs Source declination (J2000)
53- 61 F9.6 --- z ?=-9.999 Redshift
63- 70 F8.3 Mpc Dist ?=-9.999 Distance
72- 78 F7.3 [Msun] logM* ?=-99.999 Log stellar mass
80- 84 F5.3 mag W1-W2 WISE w1mpro-w2mpro color index
86- 90 F5.3 mag W2-W3 WISE w2mpro-w3mpro color index
92- 97 F6.3 [Msun] logMBH Log black hole mass
99-100 I2 --- Image ? Image number in Figure 2
101-102 A2 --- n_Image Note on Image (1)
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Note (1): Notes as follows:
* = These sources are outliers with very red WISE colors and have optical
diagnostics consistent with HII regions (Griffith et al.,
2011ApJ...736L..22G 2011ApJ...736L..22G).
** = These sources are extended and larger than the largest WISE aperture
(24.75 arcsec radius aperture) therefore the IR BH mass estimates for
these sources is only a lower limit.
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Acknowledgements:
Francine Marleau, francine.marleau(at)uikb.ac.at
(End) Francine Marleau [Univ. of Innsbruck], Patricia Vannier [CDS] 12-Apr-2017