Encouraging Team Science

Morrissey, Susan

doi:10.1021/cen-v083n047.p047

Cited by 6 publications

(6 citation statements)

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“…To address the goals of our current study of examining the evolution of the nuclear and star formation activ-ities in compact groups, a multi-wavelength coverage of the sample is essential. We cross-correlated Catalogue-A with the ultraviolet (UV) all sky survey of Galaxy Evolution Explorer (GALEX; Morrissey et al 2005), as well as the nearinfrared (NIR) and mid-infrared (MIR) surveys of 2MASS (Skrutskie et al 2006) and WISE (Wright et al 2010) respectively. Since the only selection criterion we applied was the availability of UV-to-MIR observations for a group as opposed to an individual galaxy, our sub-sample is also complete as the original Catalogue-A.…”

Section: Sample Selectionmentioning

confidence: 99%

Studying the evolution of galaxies in compact groups over the past 3 Gyr – II. The importance of environment in the suppression of star formation

Bitsakis

Dultzin

Ciesla

et al. 2016

Mon. Not. R. Astron. Soc.

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Section: Sample Selectionmentioning

confidence: 99%

Studying the evolution of galaxies in compact groups over the past 3 Gyr – II. The importance of environment in the suppression of star formation

Bitsakis

Dultzin

Ciesla

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The data sets used in this paper are taken from the GALEX sixth data release (GR6). More technical details about the GALEX instruments can be found in Morrissey (2005). We performed aperture photometry and carefully calculated the isophotal contours around each source to account for variations in the shape of the emitting region, since most of the sources have disturbed morphologies.…”

Section: Galex Datamentioning

confidence: 99%

A mid-IR study of Hickson compact groups

Bitsakis¹,

Charmandaris²,

Cunha³

et al. 2011

A&A

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We present a comprehensive study of the impact of the environment of compact galaxy groups on the evolution of their members using a multiwavelength analysis from the ultraviolet to the infrared, for a sample of 32 Hickson compact groups (HCGs) containing 135 galaxies. Fitting the spectral energy distributions (SEDs) of all galaxies with the state-of-the-art model of da Cunha et al. (2008, MNRAS, 388, 1595 we can accurately calculate their mass, SFR, and extinction, as well as estimate their infrared luminosity and dust content. We compare our findings with samples of field galaxies, early-stage interacting pairs, and cluster galaxies with similar data. We find that classifying the groups as dynamically "old" or "young", depending on whether at least one quarter of their members are early-type systems, is physical and consistent with past classifications of HCGs based on their atomic gas content. Dynamically "old" groups are more compact and display higher velocity dispersions than "young" groups. Late-type galaxies in dynamically "young" groups have specific star formation rates (sSFRs), NUV-r, and mid-infrared colors that are similar to those of field and earlystage, interacting pair spirals. Late-type galaxies in dynamically "old" groups have redder NUV-r colors, because they have likely experienced several tidal encounters in the past, thereby building up their stellar mass, and display lower sSFRs. We identify several late-type galaxies that have sSFRs and colors similar to those of elliptical galaxies, since they lost part of their gas due to numerous interactions with other group members. Also, 25% of the elliptical galaxies in these groups have bluer UV/optical colors than normal ellipticals in the field, probably due to star formation as they accreted gas from other galaxies of the group or via merging of dwarf companions. Finally, our SED modeling suggests that in 13 groups, ten of which are dynamically "old", there is diffuse cold dust in the intragroup medium. All this evidence points to an evolutionary scenario in which the effects of the group environment and the properties of the galaxy members are not instantaneous. Early on, the influence of close companions to group galaxies is similar to the one of galaxy pairs in the field. However, as the time progresses, the effects of tidal torques and minor merging shape the morphology and star formation history of the group galaxies, leading to an increase in the fraction of early-type members and a rapid build up of the stellar mass in the remaining late-type galaxies.

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“…UV-emission probes star-formation on timescales of ∼100 Myr, the lifetime of the massive OB stars. We integrated the counts per second (CPS) within each galaxy or region and then applied m FUV = −2.5 log(CPS)+18.82 (Morrissey et al 2005) to derive the magnitude in the FUV-band. We compiled the m FUV found for each galaxy in Table 2.…”

Section: Fuv Datamentioning

confidence: 99%

Massive star formation in Wolf-Rayet galaxies

López-Sánchez

2010

A&A

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Aims. We performed a comprehensive analysis of a sample of 20 starburst galaxies that show a substantial population of very young massive stars, most of them classified as Wolf-Rayet galaxies. Methods. In this paper, the last in the series, we analyze the global properties of our galaxy sample using multiwavelength data extracted from our own observations (Hα fluxes, B and H-band magnitudes) and from the literature, which include X-ray, FUV, FIR, and radio (both H i spectral line and 1.4 GHz radio-continuum) measurements.Results. The agreement between our Hα-based star-formation rates (Sfr) and those provided by indicators at other wavelengths is remarkable, but we consider that the new Hα-based calibration provided by Calzetti et al. (2007, ApJ, 666, 870) should be preferred to older calibrations. The FUV-based Sfr provides a powerful tool for analyzing the star-formation activity on both global and local scales independently to the Hα emission. We provide empirical relationships between the ionized gas mass, neutral gas mass, dust mass, stellar mass, and dynamical mass with the B-luminosity. Although all mass estimations increase with increasing luminosity, we find important deviations to the general trend in some objects, which seem to be the consequence of their particular evolutionary histories. The analysis of the mass-to-light ratios give similar results. We investigate the mass-metallicity relations and conclude that both the nature and the star-formation history are needed to understand the relationships between both properties. The majority of the galaxies follow a Schmidt-Kennicutt scaling law of star-formation that agrees with that reported in individual star-forming regions within M 51 but not with that found in normal spiral galaxies. Dwarf galaxies seem to be forming stars more efficiently than the outskirts of spiral galaxies. We find a relation between the reddening coefficient and the warm dust mass indicating that the extinction is mainly internal to the galaxies. The comparison with the closed-box model also indicates that the environment has strongly affected their evolution. Conclusions. Considering all multiwavelength data, we found that 17 up to 20 galaxies are clearly interacting or merging with lowluminosity dwarf objects or H i clouds. The remaining three galaxies (Mkn 5, SBS 1054+364, and SBS 1415+437) show considerable divergences of some properties when comparing with similar objects. Many of the interacting/merging features are only detected when deep optical spectroscopy and a detailed multiwavelength analysis, including H i observations, are obtained. We conclude that interactions do play a fundamental role in the triggering mechanism of the strong star-formation activity observed in dwarf starburst galaxies.

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Encouraging Team Science

Cited by 6 publications

References 0 publications

Studying the evolution of galaxies in compact groups over the past 3 Gyr – II. The importance of environment in the suppression of star formation

Studying the evolution of galaxies in compact groups over the past 3 Gyr – II. The importance of environment in the suppression of star formation

A mid-IR study of Hickson compact groups

Massive star formation in Wolf-Rayet galaxies

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