The Merger History, Active Galactic Nucleus, and Dwarf Galaxies of Hickson Compact Group 59

Konstantopoulos, I. S.; Gallagher, S. C.; Федотов, К. В.; Durrell, P. R.; Tzanavaris, P.; Hill, Allison R.; Zabludoff, Ann I.; Maier, Millicent; Elmegreen, D. M.; Charlton, Jane C.; Johnson, K. E.; Brandt, W. N.; Walker, Lisa May; Eracleous, Michael; Maybhate, A.; Grönwall, C.; English, Jayanne; Hornschemeier, A. E.; Mulchaey, John S.

doi:10.1088/0004-637x/745/1/30

Cited by 13 publications

(14 citation statements)

References 90 publications

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“…In optical and molecular observations of M51, Bastian et al (2005a) find that star cluster complexes are young (< 10 Myr) and have a strong correlation between mass and size (unlike for isolated star clusters) which is similar to that found for GMCs. In studies of Hickson Compact Group galaxies, Konstantopoulos et al (2012) find a linear relation in HCG 59, but no relation for HCG 7 (Konstantopoulos et al 2010).…”

Section: Star Cluster Complexes In Eastern Tailmentioning

confidence: 96%

Tidal Tails of Minor Mergers. Ii. Comparing Star Formation in the Tidal Tails of NGC 2782

Knierman

Scowen

Veach

et al. 2013

ApJ

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The peculiar spiral NGC 2782 is the result of a minor merger with a mass ratio ∼ 4 : 1 occurring ∼ 200 Myr ago. This merger produced a molecular and Hi rich, optically bright Eastern tail and an Hi-rich, optically faint Western tail. Non-detection of CO in the Western Tail by Braine et al. (2001) suggested that star formation had not yet begun. However, deep UBV R and Hα narrowband images show evidence of recent star formation in the Western tail, though it lacks massive star clusters and cluster complexes. Using Herschel PACS spectroscopy, we discover 158µm [Cii] emission at the location of the three most luminous Hα sources in the Eastern tail, but not at the location of the even brighter Hα source in the Western tail. The Western tail is found to have a normal star formation efficiency (SFE), but the Eastern tail has a low SFE. The lack of CO and [Cii] emission suggests the Western tail Hii region may have a low carbon abundance and be undergoing its first star formation. The Western tail is more efficient at forming stars, but lacks massive clusters. We propose that the low SFE in the Eastern tail may be due to its formation as a splash region where gas heating is important even though it has sufficient molecular and neutral gas to make massive star clusters. The Western tail, which has lower gas surface density and does not form high mass star clusters, is a tidally formed region where gravitational compression likely enhances star formation.

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Section: Star Cluster Complexes In Eastern Tailmentioning

confidence: 96%

Tidal Tails of Minor Mergers. Ii. Comparing Star Formation in the Tidal Tails of NGC 2782

Knierman

Scowen

Veach

et al. 2013

ApJ

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“…59B E ✓ Western string of H II regions; tidal bridge to A (Konstantopoulos et al 2012). 92D E ✓ Prominent tidal tails (TF09) and diffuse emission.…”

Section: X Versus M *mentioning

confidence: 99%

Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

Tzanavaris

Hornschemeier²,

Gallagher

et al. 2016

ApJ

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We obtain total galaxy X-ray luminosities, L X , originating from individually detected point sources in a sample of 47 galaxies in 15 compact groups of galaxies (CGs). For the great majority of our galaxies, we find that the detected point sources most likely are local to their associated galaxy, and are thus extragalactic X-ray binaries (XRBs) or nuclear active galactic nuclei (AGNs). For spiral and irregular galaxies, we find that, after accounting for AGNs and nuclear sources, most CG galaxies are either within the ±1σ scatter of the Mineo et al. L X -star formation rate (SFR) correlation or have higher L X than predicted by this correlation for their SFR. We discuss how these "excesses" may be due to low metallicities and high interaction levels. For elliptical and S0 galaxies, after accounting for AGNs and nuclear sources, most CG galaxies are consistent with the Boroson et al. L X -stellar mass correlation for low-mass XRBs, with larger scatter, likely due to residual effects such as AGN activity or hot gas. Assuming non-nuclear sources are low-or high-mass XRBs, we use appropriate XRB luminosity functions to estimate the probability that stochastic effects can lead to such extreme L X values. We find that, although stochastic effects do not in general appear to be important, for some galaxies there is a significant probability that high L X values can be observed due to strong XRB variability.

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“…The lack of low mass star-forming galaxies could in part also be due to selection -there is a lower limit to galaxies identified as belonging to the group, though we do not see mid-IR canyon in LVL+SINGS, which has a similar population of galaxies, as shown in Figure 1. Lower mass, star-forming galaxies are likely to be farther away from the core, and so again could be missed in the selection, like the star-forming dwarfs found on the outskirts of HCG 59 (Konstantopoulos et al 2012). It is not clear which effect dominates, the dearth of mid-IR transition galaxies is likely due to some combination of these factors.…”

Section: Implications For Galaxy Evolutionmentioning

confidence: 99%

The Optical Green Valley Versus Mid-Infrared Canyon in Compact Groups

Walker

Butterfield

Johnson

et al. 2013

ApJ

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Compact groups of galaxies provide conditions similar to those experienced by galaxies in the earlier universe. Recent work on compact groups has led to the discovery of a dearth of mid-infrared transition galaxies (MIRTGs) in IRAC (3.6-8.0 µm) color space (Johnson et al. 2007;Walker et al. 2012) as well as at intermediate specific star formation rates (Tzanavaris et al. 2010). However, we find that in compact groups these mid-infrared (mid-IR) transition galaxies in the mid-infrared dearth have already transitioned to the optical ([g-r]) red sequence. We investigate the optical color-magnitude diagram (CMD) of 99 compact groups containing 348 galaxies and compare the optical CMD with mid-IR color space -2 -for compact group galaxies. Utilizing redshifts available from SDSS, we identified new galaxy members for 6 groups. By combining optical and mid-IR data, we obtain information on both the dust and the stellar populations in compact group galaxies. We also compare with more isolated galaxies and galaxies in the Coma cluster, which reveals that, similar to clusters, compact groups are dominated by optically red galaxies. While we find that compact group transition galaxies lie on the optical red sequence, LVL+SINGS mid-IR transition galaxies span the range of optical colors. The dearth of mid-IR transition galaxies in compact groups may be due to a lack of moderately star forming low mass galaxies; the relative lack of these galaxies could be due to their relatively small gravitational potential wells. This makes them more susceptible to this dynamic environment, thus causing them to more easily lose gas or be accreted by larger members.

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The Merger History, Active Galactic Nucleus, and Dwarf Galaxies of Hickson Compact Group 59

Cited by 13 publications

References 90 publications

Tidal Tails of Minor Mergers. Ii. Comparing Star Formation in the Tidal Tails of NGC 2782

Tidal Tails of Minor Mergers. Ii. Comparing Star Formation in the Tidal Tails of NGC 2782

Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

The Optical Green Valley Versus Mid-Infrared Canyon in Compact Groups

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