GHASP: An H<i>α</i> kinematic survey of spiral and irregular galaxies

Garrido, O.; Marcelin, M.; Amram, P.; Boulesteix, J.

doi:10.1051/0004-6361:20020479

Cited by 83 publications

(92 citation statements)

References 12 publications

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“…Note however that the accuracy of measurements of i given by Garrido et al (2002) is rather low, ±(5 • −10 • ).…”

Section: Ngc 3893mentioning

confidence: 99%

“…The orientation angles of this galaxy were also estimated from the Hα velocity field by Garrido et al (2002), by minimizing the dispersion of the points along the rotation curve.…”

Section: Ngc 3893mentioning

confidence: 99%

“…The largest project of this type is the GHASP survey, carried out at the Haute-Provence Observatory, which should provide a homogeneous sample of 2D velocity fields of about 200 spiral and irregular galaxies. This survey aimes to compare galaxies in different environments, different stages of evolution and at different redshifts (Garrido et al 2002(Garrido et al , 2003. Unlike the works mentioned above, the main goal of our project is to study the regular deviations of gas motion from circular rotation in spiral galaxies, which may be caused by spiral density wavesin parallel with the routine task of obtaining the rotation curves and mass distributions.…”

Section: Introductionmentioning

confidence: 99%

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The orientation parameters and rotation curves of 15 spiral galaxies

Fridman

Afanasiev

Додонов

et al. 2005

A&A

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Abstract. We analyzed ionized gas motion and disk orientation parameters for 15 spiral galaxies. Their velocity fields were measured with the Hα emission line by using the Fabry-Perot interferometer at the 6 m telescope of SAO RAS. Special attention is paid to the problem of estimating the position angle of the major axis (PA 0 ) and the inclination (i) of a disk, which strongly affect the derived circular rotation velocity. We discuss and compare different methods of obtaining these parameters from kinematic and photometric observations, taking into account the presence of regular velocity (brightness) perturbations caused by spiral density waves. It is shown that the commonly used method of tilted rings may lead to systematic errors in the estimation of orientation parameters (and hence of circular velocity) being applied to galaxies with an ordered spiral structure. Instead we recommend using an assumption of constancy of i and PA 0 along a radius, to estimate these parameters. For each galaxy of our sample we present monochromatic Hα-and continuum maps, velocity fields of ionized gas, and the mean rotation curves in the frame of a model of pure circular gas motion. Significant deviations from circular motion with amplitudes of several tens of km s −1 (or higher) are found in almost all galaxies. The character and possible nature of the non-circular motion are briefly discussed.

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“…Note however that the accuracy of measurements of i given by Garrido et al (2002) is rather low, ±(5 • −10 • ).…”

Section: Ngc 3893mentioning

confidence: 99%

“…The orientation angles of this galaxy were also estimated from the Hα velocity field by Garrido et al (2002), by minimizing the dispersion of the points along the rotation curve.…”

Section: Ngc 3893mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The orientation parameters and rotation curves of 15 spiral galaxies

Fridman

Afanasiev

Додонов

et al. 2005

A&A

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“…We supplemented our sample by adding host galaxies whose rotation sense was determined from the spectroscopic observations in the literature (Rubin et al 1982(Rubin et al , 1985(Rubin et al , 1999Broeils & van Woerden 1994;Han et al 1995;Taylor et al 1995;Rhee & van Albada 1996;Zaritsky et al 1997;Sofue 1997;Sofue et al 1997Sofue et al , 1998Sofue et al , 2003Héraudeau & Simien 1998;Héraudeau et al 1999;Vega Beltrán et al 2001;Garrido et al 2002Garrido et al , 2003Garrido et al , 2004Garrido et al , 2005Vogt et al 2004;Coccato et al 2004;Fridman et al 2005;Hernandez et al 2005;Noordermeer et al 2005;Chemin et al 2006;Falcón-Barroso et al 2006;Daigle et al 2006;Ganda et al 2006;Azzaro et al 2006;Herbert-Fort et al 2008;Epinat et al 2008aEpinat et al , 2008bSwaters et al 2009). We compiled 390 satellites associated with 116 hosts.…”

Section: Spin Direction Of Host Galaxiesmentioning

confidence: 99%

Orbital Dependence of Galaxy Properties in Satellite Systems of Galaxies

Hwang

Park

2010

ApJ

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We study the dependence of satellite galaxy properties on the distance to the host galaxy and the orbital motion (prograde and retrograde orbits) using the Sloan Digital Sky Survey (SDSS) data. From SDSS Data Release 7, we find 3515 isolated satellite systems of galaxies at z < 0.03 that contain 8904 satellite galaxies. Using this sample, we construct a catalog of 635 satellites associated with 215 host galaxies whose spin directions are determined by our inspection of the SDSS color images and/or by spectroscopic observations in the literature. We divide satellite galaxies into prograde and retrograde orbit subsamples depending on their orbital motion with respect to the spin direction of the host. We find that the number of galaxies in prograde orbit is nearly equal to that of retrograde orbit galaxies: the fraction of satellites in prograde orbit is 50% ± 2%. The velocity distribution of satellites with respect to their hosts is found to be almost symmetric: the median bulk rotation of satellites is −1 ± 8 km s −1 . It is found that the radial distribution of early-type satellites in prograde orbit is strongly concentrated toward the host while that of retrograde ones shows much less concentration. We also find the orbital speed of late-type satellites in prograde orbit increases as the projected distance to the host (R) decreases while the speed decreases for those in retrograde orbit. At R less than 0.1 times the host virial radius (R < 0.1r vir,host ), the orbital speed decreases in both prograde and retrograde orbit cases. Prograde satellites are on average fainter than retrograde satellites for both early and late morphological types. The u − r color becomes redder as R decreases for both prograde and retrograde orbit late-type satellites. The differences between prograde and retrograde orbit satellite galaxies may be attributed to their different origin or the different strength of physical processes that they have experienced through hydrodynamic interactions with their host galaxies.

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“…The GHASP sample consists of 203 spiral and irregular galaxies in the local universe for which high-resolution Hα maps have been observed with Fabry-Perot interferometry (Garrido et al 2002(Garrido et al , 2003Garrido, Marcelin, & Amram 2004;Garrido et al 2005;Spano et al 2008;Epinat et al 2010;Torres-Flores et al 2011). The GHASP sample was initially designed to be a subsample of the Westerbork survey (WHISP, van der Hulst, van Albada, & Sancisi 2001) with the goal of providing a local universe reference for kinematics and dynamics of disk-like galaxies.…”

Section: The Ghasp Samplementioning

confidence: 99%

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theR_cband

Barbosa

Oliveira

Amram

et al. 2015

Mon. Not. R. Astron. Soc.

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We present R c -band surface photometry for 170 of the 203 galaxies in GHASP, Gassendi H-Alpha survey of SPirals, a sample of late-type galaxies for which high-resolution FabryPerot H maps have previously been obtained. Our data set is constructed by new R c -band observations taken at the Observatoire de Haute-Provence (OHP), supplemented with Sloan Digital Sky Survey (SDSS) archival data, obtained with the purpose of deriving homogeneous photometric profiles and parameters. Our results include R c -band surface brightness profiles for 170 galaxies and ugriz profiles for 108 of these objects. We catalogue several parameters of general interest for further reference, such as total magnitude, effective radius and isophotal parameters -magnitude, position angle, ellipticity and inclination. We also perform a structural decomposition of the surface brightness profiles using a multi-component method in order to separate disks from bulges and bars, and to observe the main scaling relations involving luminosities, sizes and maximum velocities.We determine the R c -band Tully Fisher relation using maximum velocities derived solely from Hα rotation curves for a sample of 80 galaxies, resulting in a slope of −8.1 ± 0.5, zero point of −3.0 ± 1.0 and an estimated intrinsic scatter of 0.28 ± 0.07. We note that, different from the TF-relation in the near-infrared derived for the same sample, no change in the slope of the relation is seen at the low-mass end (for galaxies with V max < 125 km/s). We suggest that this different behaviour of the Tully Fisher relation (with the optical relation being described by a single power-law while the near-infrared by two) may be caused by differences in the stellar mass to light ratio for galaxies with V max < 125 km/s.

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GHASP: An Hα kinematic survey of spiral and irregular galaxies

Cited by 83 publications

References 12 publications

The orientation parameters and rotation curves of 15 spiral galaxies

The orientation parameters and rotation curves of 15 spiral galaxies

Orbital Dependence of Galaxy Properties in Satellite Systems of Galaxies

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theR_cband

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GHASP: An Hα kinematic survey of spiral and irregular galaxies

Cited by 83 publications

References 12 publications

The orientation parameters and rotation curves of 15 spiral galaxies

The orientation parameters and rotation curves of 15 spiral galaxies

Orbital Dependence of Galaxy Properties in Satellite Systems of Galaxies

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theRcband

Contact Info

Product

Resources

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GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theR_cband