Dipartimento di Astronomia e Scienza dello Spazio, Università degli Studi di Firenze, Largo E.Fermi 2, 50125 Firenze, Italy e-mail: email@example.com
2 INAF - Osservatorio Astrofisico di Arcetri, Largo E.Fermi 5, 50125 Firenze, Italy
3 INAF - Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Italy
4 Department of Physics, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, NY 14623, USA
5 Damir, Instituto de Estructura de la Materia, CSIC, Serrano 121, 28006 Madrid, Spain
6 School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK
7 Institute of Astronomy, Physics Department, ETH, Zurich, Switzerland
8 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
9 ESA Research and Space Science Department
10 Department of Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
Accepted: 14 February 2007
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, NGC 4303, NGC 3310 and NGC 4258. The bright optical emission lines Hα λ , [NII] λλ and [SII] λλ were used to study the kinematics of the ionized gas in the nuclear region of each galaxy with a ~ 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 NGC 3310, 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 – at the 95% confidence level. In NGC 4303 the kinematical data require the presence of a BH with mass (for a disk inclination deg) 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 – at the 95% confidence level. In NGC 4258, the observed kinematics require the presence of a black hole with ( deg) and, taking into account reasonable limits for the inclination, MBH is in the range – at the 95% confidence level. This result is in good agreement with the published value , derived from H2O-maser observations. As in the case of NGC 4303, 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 NGC 4258, has been successful.
Key words: black hole physics / galaxies: spiral / galaxies: bulges / Galaxy: kinematics and dynamics / galaxies: nuclei
Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with proposal 8228.
© ESO, 2007