An investigation of star formation and dust attenuation in major mergers using ultraviolet and infrared data

Yuan, Fang-Ting; Takeuchi, Tsutomu T.; Matsuoka, Yoshiki; Buat, V.; Burgarella, D.; Iglésias-Páramo, J.

doi:10.1051/0004-6361/201220451

Cited by 24 publications

(20 citation statements)

References 70 publications

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“…3.2). This agrees with previous observational studies (e.g., Ellison et al 2008;Yuan et al 2012), as well as with numerical simulations (e.g., Hopkins et al 2013;Moreno et al 2015). These studies indicate that tidally induced star formation becomes evident in the central region of the galaxies as a consequence of gas inflows.…”

Section: Resultssupporting

confidence: 92%

Central star formation and metallicity in CALIFA interacting galaxies

Barrera-Ballesteros

Sánchez

García-Lorenzo

et al. 2015

A&A

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We use optical integral-field spectroscopic (IFS) data from 103 nearby galaxies at different stages of the merging event, from close pairs to merger remnants provided by the CALIFA survey, to study the impact of the interaction in the specific star formation and oxygen abundance on different galactic scales. To disentangle the effect of the interaction and merger from internal processes, we compared our results with a control sample of 80 non-interacting galaxies. We confirm the moderate enhancement (×2-3 times) of specific star formation for interacting galaxies in central regions as reported by previous studies; however, the specific star formation is comparable when observed in extended regions. We find that control and interacting star-forming galaxies have similar oxygen abundances in their central regions, when normalized to their stellar masses. Oxygen abundances of these interacting galaxies seem to decrease compared to the control objects at the large aperture sizes measured in effective radius. Although the enhancement in central star formation and lower metallicities for interacting galaxies have been attributed to tidally induced inflows, our results suggest that other processes such as stellar feedback can contribute to the metal enrichment in interacting galaxies.

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Section: Resultssupporting

confidence: 92%

Central star formation and metallicity in CALIFA interacting galaxies

Barrera-Ballesteros

Sánchez

García-Lorenzo

et al. 2015

A&A

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“…The open question of whether merging is a major contributor to the cosmic star formation history (SFH) has been tackled in different ways: Do merging galaxies have higher star formation rates compared to isolated ones (Ellison et al 2008;Patton et al 2011;Scudder et al 2012;Xu et al 2012b;Yuan et al 2012;Patton et al 2013;Lackner et al 2014)? At each epoch, are star-forming galaxies primarily mergers or isolated disks (Genzel et al 2008;Shapiro et al 2008;Förster Schreiber et al 2009;Law et al 2009;Kaviraj et al 2013a,b;Kaviraj 2014a,b)?…”

Section: Merger Contribution To Cosmic Star Formationmentioning

confidence: 99%

RESOLVING THE DISCREPANCY OF GALAXY MERGER FRACTION MEASUREMENTS AT z ∼ 0–3

Man

Zirm

Toft

2016

ApJ

137

191

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We measure the merger fraction of massive galaxies using the UltraVISTA/COSMOS Ks-band selected catalog, complemented with the deeper, higher resolution 3DHST+CANDELS catalog selected in the HST /WFC3 H -band, presenting the largest mass-complete photometric merger sample up to z ∼ 3. We find that selecting mergers using the H 160 -band flux ratio leads to an increasing merger fraction with redshift, while selecting mergers using the stellar mass ratio causes a diminishing redshift dependence. Defining major and minor mergers as having stellar mass ratios of 1:1 -4:1 and 4:1 -10:1 respectively, the results imply ∼1 major and 1 minor merger for an average massive (log(M ⋆ /M ⊙ ) 10.8) galaxy during z = 0.1 − 2.5. There may be an additional ∼ 0.5(0.3) major (minor) merger if we use the H-band flux ratio selection. The observed amount of major merging alone is sufficient to explain the observed number density evolution for the very massive (log(M ⋆ /M ⊙ ) 11.1) galaxies. We argue that these very massive galaxies can put on a maximum of 6% of stellar mass in addition to major and minor merging, so that their number density evolution remains consistent with observations. The observed number of major and minor mergers can increase the size of a massive quiescent galaxy by a factor of two at most. This amount of merging is enough to bring the compact quiescent galaxies formed at z > 2 to lie at 1σ below the mean of the stellar mass-size relation as measured in some works (e.g. Newman et al. 2012), but additional mechanisms are needed to fully explain the evolution, and to be consistent with works suggesting stronger evolution (e.g. van der Wel et al. 2014).

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“…The SFR is derived from L IR using the formula of Kennicutt (1998), with an additional correction factor of -10 0.20 for the conversion from the Salpeter IMF to the Kroupa IMF (Calzetti 2013). It is worth noting that this formalism misses the contribution from unobscured UV radiation, which is on the order of 20% for KPAIR galaxies (Yuan et al 2012). It is also contaminated by the dust emission powered by the radiation of old stars (Buat & Xu 1996).…”

Section: Dust Mass L Ir and Stellar Massmentioning

confidence: 99%

HERSCHEL OBSERVATIONS OF MAJOR MERGER PAIRS AT z = 0: DUST MASS AND STAR FORMATION

Cao

Domingue

et al. 2016

ApJS

101

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We present Herschel PACS and SPIRE far-infrared (FIR) and submillimeter imaging observations for a large K-band selected sample of 88 close major-merger pairs of galaxies (H-KPAIRs) in 6 photometric bands (70, 100, 160, 250, 350, and 500 μm). Among 132 spiral galaxies in the 44 spiral-spiral (S+S) pairs and 44 spiral-elliptical (S+E) pairs, 113 are detected in at least 1 Herschel band. The star formation rate (SFR) and dust mass (M dust ) are derived from the IR SED fitting. The mass of total gas (M gas ) is estimated by assuming a constant dust-to-gas mass ratio of 0.01. Star-forming spiral galaxies (SFGs) in S+S pairs show significant enhancements in both specific star formation rate (sSFR) and star formation efficiency (SFE), while having nearly the same gas mass compared to control galaxies. On the other hand, for SFGs in S+E pairs, there is no significant sSFR enhancement and the mean SFE enhancement is significantly lower than that of SFGs in S+S pairs. This suggests an important role for the disk-disk collision in the interaction-induced star formation. The M gas of SFGs in S+E pairs is marginally lower than that of their counterparts in both S+S pairs and the control sample. Paired galaxies with and without interaction signs do not differ significantly in their mean sSFR and SFE. As found in previous works, this much larger sample confirms that the primary and secondary spirals in S+S pairs follow a Holmberg effect correlation on sSFR.

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An investigation of star formation and dust attenuation in major mergers using ultraviolet and infrared data

Cited by 24 publications

References 70 publications

Central star formation and metallicity in CALIFA interacting galaxies

Central star formation and metallicity in CALIFA interacting galaxies

RESOLVING THE DISCREPANCY OF GALAXY MERGER FRACTION MEASUREMENTS AT z ∼ 0–3

HERSCHEL OBSERVATIONS OF MAJOR MERGER PAIRS AT z = 0: DUST MASS AND STAR FORMATION

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