Multi-wavelength study of a new sample of blue compact dwarf galaxies

Петросян, А. Р.; Movsessian, T. A.; Comte, G.; Kunth, D.; Додонов, С. Н.

doi:10.1051/0004-6361:20020819

Cited by 13 publications

(19 citation statements)

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“…Only for Mrk 32 and Tololo 1434+032 we found that the distribution of the gaseous emission differs considerably from that of the stellar component. Spatial discrepancies in the distribution of emission lines and continuum are interpreted as signs of a spatial migration of the SF over the history of the galaxies (Petrosian et al 2002). However, small spatial offsets between continuum and emission line peaks, as those seen in Tololo 1434+032, and which are indeed a common feature in compact starburst galaxies (Hunter & Thronson 1995;Maiz-Apellaniz et al 1998;Lagos et al 2007), are likely related to the release of kinetic energy by massive stars and supernova explosions.…”

Section: Discussionmentioning

confidence: 96%

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Mapping the properties of blue compact dwarf galaxies: integral field spectroscopy with PMAS

Cairós

Caon

Zurita

et al. 2010

A&A

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Context. Blue compact dwarf (BCD) galaxies are low-luminosity, low-metal content dwarf systems undergoing violent bursts of star formation. They present a unique opportunity to probe galaxy formation and evolution and to investigate the process of star formation in a relatively simple scenario. Spectrophotometric studies of BCDs are essential to disentangle and characterize their stellar populations. Aims. We perform integral field spectroscopy of a sample of BCDs with the aim of analyzing their morphology, the spatial distribution of some of their physical properties (excitation, extinction, and electron density) and their relationship with the distribution and evolutionary state of the stellar populations. Methods. Integral field spectroscopy observations of the sample galaxies were carried out with the Potsdam Multi-Aperture Spectrophotometer (PMAS) at the 3.5 m telescope at Calar Alto Observatory. An area 16 × 16 in size was mapped with a spatial sampling of 1 × 1 . We obtained data in the 3590−6996 Å spectral range, with a linear dispersion of 3.2 Å per pixel. From these data we built two-dimensional maps of the flux of the most prominent emission lines, of two continuum bands, of the most relevant line ratios, and of the gas velocity field. Integrated spectra of the most prominent star-forming regions and of whole objects within the FOV were used to derive their physical parameters and the gas metal abundances. Results. Six galaxies display the same morphology both in emission line and in continuum maps; only in two objects, Mrk 32 and Tololo 1434+032, the distributions of the ionized gas and of the stars differ considerably. In general the different excitation maps for a same object display the same pattern and trace the star-forming regions, as expected for objects ionized by hot stars; only the outer

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Section: Discussionmentioning

confidence: 96%

“…Doublier et al (1997), Doublier et al (1999), Gil de Paz et al (2003 and Gil de Paz & Madore (2005). It is also included in the spectroscopy study of BCDs by , , Kong et al (2003), Kong (2004) and Shi et al (2005), and is the only object in our sample in common with the sample of galaxies studied by means of IFS by Petrosian et al (2002).…”

Section: Mrk 475mentioning

confidence: 99%

Mapping the properties of blue compact dwarf galaxies: integral field spectroscopy with PMAS

Cairós

Caon

Zurita

et al. 2010

A&A

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“…Also, some galaxies in the local universe are found showing regular kinematics with an HI polar disk (perpendicular to the stellar disk) (van Gorkom & Schiminovich 1997;Stanonik et al 2009). Petrosian et al (2002) observed 18 blue compact dwarf galaxies and for 8 of these they found strong misalignments between the photometric and kinematic position angles although the isovelocity contours do not indicate strong irregularities in gas motions. There are even merger remnants in the local universe that have very regular gas velocity fields such as NGC 3921 (Hibbard & van Gorkom 1996).…”

Section: The Fraction Of Irregular Gas Kinematicsmentioning

confidence: 97%

Internal kinematics of spiral galaxies in distant clusters

Kutdemir

Ziegler

Peletier³

et al. 2010

A&A

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Aims. We trace the interaction processes of galaxies at intermediate redshift by measuring the irregularity of their ionized gas kinematics, and investigate these irregularities as a function of the environment (cluster versus field) and of morphological type (spiral versus irregular). Methods. We obtain the gas velocity fields by placing three parallel and adjacent VLT/FORS2 slits on each galaxy. To quantify irregularities in the gas kinematics, we use three indicators: the standard deviation of the kinematic position angle (σ PA ), the mean deviation of the line of sight velocity profile from the cosine form which is measured using high order Fourier terms (k 3,5 /k 1 ) and the average misalignment between the kinematical and photometric major axes (Δφ). These indicators are then examined together with some photometric and structural parameters (measured from HST and FORS2 images in the optical) such as the disk scale length, rest-frame colors, asymmetry, concentration, Gini coefficient and M 20 . Our sample consists of 92 distant galaxies. 16 cluster (z ∼ 0.3 and z ∼ 0.5) and 29 field galaxies (0.10 ≤ z ≤ 0.91, mean z = 0.44) of these have velocity fields with sufficient signal to be analyzed. To compare our sample with the local universe, we also analyze a sample from the SINGS survey. Results. We find that the fraction of galaxies that have irregular gas kinematics is remarkably similar in galaxy clusters and in the field at intermediate redshifts (according to σ PA ≈ 10%, k 3,5 /k 1 ≈ 30%, Δφ ≈ 70%). The distribution of the field and cluster galaxies in (ir)regularity parameters space is also similar. On the other hand galaxies with small central concentration of light, that we see in the field sample, are absent in the cluster sample. We find that field galaxies at intermediate redshifts have more irregular velocity fields as well as more clumpy and less centrally concentrated light distributions than their local counterparts. Comparison with a SINS sample of 11 z ∼ 2 galaxies shows that these distant galaxies have more irregular gas kinematics than our intermediate redshift cluster and field sample. We do not find a dependence of the irregularities in gas kinematics on morphological type. We find that two different indicators of star formation correlate with irregularity in the gas kinematics. Conclusions. More irregular gas kinematics, also more clumpy and less centrally concentrated light distributions of spiral field galaxies at intermediate redshifts in comparison to their local counterparts indicate that these galaxies are probably still in the process of building their disks via mechanisms such as accretion and mergers. On the other hand, they have less irregular gas kinematics compared to galaxies at z ∼ 2.

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“…The latter authors (C01b) also computed optical color maps, and disclosed in deep Hα images a complex morphology of the ionized gas, most notably a large supershell expanding to the northwest of the starburst region. The Hα intensity was found to peak in between the pair of bright SF regions a and b (C01b, Petrosian et al 2002). In its LSB periphery, Mkn 324 is delimited by regular outer isophotes, and shows no conspicuous signatures of a strong gravitative perturbation.…”

Section: Mkn 324 (Ugca 439)mentioning

confidence: 99%

New insights to the photometric structure of Blue Compact Dwarf Galaxies from deep near-infrared studies

Noeske

Papaderos²,

Cairós³

et al. 2004

A&A

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Abstract. This paper is part of a series of publications which present a systematic study of Blue Compact Dwarf (BCD) Galaxies in the near infrared (NIR). Compared to the visible light, NIR data allow a better separation of the starburst emission from the light distribution of the old stellar low-surface brightness (LSB) host galaxy. We analyze deep NIR broad band images of a sample of 11 BCDs, observed with the Calar Alto 3.6 m telescope. This work enlarges the samples presented in preceding papers of this study (Noeske et al. 2003, A&A, 410, 481; Cairós et al. 2003, ApJ, 593, 312) by BCDs of the most common morphological type, displaying a regular elliptical LSB host galaxy. The data presented here allow the detection and quantitative study of the extended stellar LSB host galaxy in all sample BCDs. The NIR surface brightness profiles (SBPs) of the LSB host galaxies agree at large galactocentric radii with those from optical studies, showing also an exponential intensity decrease and compatible scale lengths. Similar to Noeske et al. (2003), we find centrally flattening exponential (type V) SBPs of the host galaxy for several BCDs. Such SBPs remain mostly undetected in optical bands, due to the comparatively stronger starburst emission at these wavelengths. We apply a modified exponential distribution to decompose and quantitatively analyze SBPs of LSB hosts with a type V intensity distribution. We present the results of the surface photometry and the decomposition of SBPs, and discuss individual objects with respect to morphological details of their star-forming regions.

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Multi-wavelength study of a new sample of blue compact dwarf galaxies

Cited by 13 publications

References 50 publications

Mapping the properties of blue compact dwarf galaxies: integral field spectroscopy with PMAS

Mapping the properties of blue compact dwarf galaxies: integral field spectroscopy with PMAS

Internal kinematics of spiral galaxies in distant clusters

New insights to the photometric structure of Blue Compact Dwarf Galaxies from deep near-infrared studies

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