2007A&A...469..405P


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.11CEST08:56:07

2007A&A...469..405P - Astronomy and Astrophysics, volume 469, 405-423 (2007/7-2)

Supermassive black holes in the Sbc spiral galaxies NGC 3310, NGC 4303 and NGC 4258.

PASTORINI G., MARCONI A., CAPETTI A., AXON D.J., ALONSO-HERRERO A., ATKINSON J., BATCHELDOR D., CAROLLO C.M., COLLETT J., DRESSEL L., HUGHES M.A., MACCHETTO D., MACIEJEWSKI W., SPARKS W. and VAN DER MAREL R.

Abstract (from CDS):

We have undertaken an HST Space Telescope Imaging Spectrograph survey of 54 late type spiral galaxies to study the scaling relations between black holes and their host spheroids at the low mass end. Our aim is to measure black hole masses or to set upper limits for a sizeable sample of spiral galaxies. In this paper we present new Space Telescope Imaging Spectrograph (STIS) observations of three spiral galaxies, NGC4303, NGC3310 and NGC4258. The bright optical emission lines Hα λ 6564Å, [NII] λλ 6549,6585Å and [SII] λλ 6718,6732Å were used to study the kinematics of the ionized gas in the nuclear region of each galaxy with a ∼0.07" spatial resolution. Our STIS data for NGC 4258 were analyzed in conjunction with archival ones to compare the gas kinematical estimate of the black hole mass with the accurate value from H2O-maser observations. In NGC3310, the observed gas kinematics is well matched by a circularly rotating disk model but we are only able to set an upper limit to the BH mass which, taking into account the allowed disk inclinations, varies in the range 5.0x106-4.2x107M at the 95% confidence level. In NGC4303 the kinematical data require the presence of a BH with mass MBH=(5.0)+0.87–2.26x106M (for a disk inclination i=70deg) but the weak agreement between data and disk model does not allow us to consider this measurement completely reliable. If the allowed inclination values are taken into account, MBH varies in the range 6.0x105-1.6x107M at the 95% confidence level. In NGC 4258, the observed kinematics require the presence of a black hole with MBH=(7.9)+6.2–3.5x107M (i=60deg) and, taking into account reasonable limits for the inclination, MBH is in the range 2.5x107-2.6x108M at the 95% confidence level. This result is in good agreement with the published value (3.9±0.1)x107M, derived from H2O-maser observations. As in the case of NGC4303, the agreement between observed and model kinematics is not strong but this does not affect the recovery of the correct MBH value. Our attempt at measuring BH masses in these 3 late type Sbc spiral galaxies has shown that these measurements are very challenging and at the limit of the highest spatial resolution currently available. Nonetheless our estimates are in good agreement with the scaling relations between black holes and their host spheroids suggesting that (i) they are reliable and (ii) black holes in spiral galaxies follow the same scaling relations as those in more massive early-type galaxies. A crucial test for the gas kinematical method, the correct recovery of the known BH mass in NGC4258, has been successful.

Abstract Copyright:

Journal keyword(s): black hole physics - galaxies: spiral - galaxies: bulges - Galaxy: kinematics and dynamics - galaxies: nuclei

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 1300 GiP 03 19 41.0453355271 -19 24 40.141850719   11.16 10.42 9.90 10.7 ~ 459 0
2 NGC 2748 GiG 09 13 43.037 +76 28 31.23   11.7       ~ 182 0
3 M 81 Sy2 09 55 33.17306143 +69 03 55.0609270   7.89 6.94     ~ 4055 5
4 NGC 3310 AGN 10 38 45.857 +53 30 11.89   12.45 12.15     ~ 745 1
5 M 105 LIN 10 47 49.600 +12 34 53.87   10.56 9.76 9.12 8.18 ~ 1397 0
6 NGC 4041 SyG 12 02 12.2373728821 +62 08 14.095878409   11.6       ~ 234 1
7 M 106 Sy2 12 18 57.620 +47 18 13.39   9.14 8.41 8.11   ~ 2179 3
8 M 61 Sy2 12 21 54.9275149050 +04 28 25.588335799 10.07 10.18 9.65     ~ 901 2
9 NGC 4335 rG 12 23 01.908 +58 26 40.96   13.7       ~ 77 1
10 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 6008 0
11 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 4087 3
12 NAME Ursa Major Cluster ClG 15 08.8 +67 07           ~ 389 0
13 IC 1459 GiP 22 57 10.60677155 -36 27 43.9953697   10.96 11.85 9.34 10.3 ~ 586 2
14 NAME Local Group GrG ~ ~           ~ 7226 0

    Equat.    Gal    SGal    Ecl

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