Is HCG 31 undergoing a merger or a fly-by interaction?

Richer, M. G.; Георгиев, Л.; Rosado, M.; Bullejos, A.; Valdez-Gutiérrez, Margarita; Dultzin‐Hacyan, D.

doi:10.1051/0004-6361:20021394

Cited by 15 publications

(63 citation statements)

References 42 publications

(140 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Rubin, Hunter, & Ford (1990) concur, identifying two overlapping strongly interacting edge-on disk galaxies (A and C), another edge-on galaxy (B), and a fainter galaxy (D), as well as other more distant galaxies. In contrast, Richer et al (2003) conclude that A and C are a single tidally distorted galaxy, and some of the more distant objects are tidal debris rather than pre-existing galaxies. They find that Galaxy B is kinematically distinct from A+C and is counter-rotating relative to it, thus they conclude that another more distant galaxy (G) is responsible for the tidal features of A+C.…”

Section: 78±mentioning

confidence: 71%

Diffuse X-Ray-emitting Gas in Major Mergers

Smith

Campbell

Struck

et al. 2018

View full text Add to dashboard Cite

Using archived data from the Chandra X-ray telescope, we have extracted the diffuse Xray emission from 49 equal-mass interacting/merging galaxy pairs in a merger sequence, from widely separated pairs to merger remnants. After removal of contributions from unresolved point sources, we compared the diffuse thermal X-ray luminosity from hot gas (L X (gas)) with the global star formation rate (SFR). After correction for absorption within the target galaxy, we do not see strong trend of L X (gas)/SFR with SFR or merger stage for galaxies with SFR > 1 M ⊙ yr −1 . For these galaxies, the median L X (gas)/SFR is 5.5 × 10 39 ((erg s −1 )/M ⊙ yr −1 )), similar to that of normal spiral galaxies. These results suggest that stellar feedback in star forming galaxies reaches an approximately steady state condition, in which a relatively constant fraction of about 2% of the total energy output from supernovae and stellar winds is converted into X-ray flux. Three late-stage merger remnants with low SFRs and high K band luminosities (L K ) have enhanced L X (gas)/SFR; their UV/IR/optical colors suggest that they are post-starburst galaxies, perhaps in the process of becoming ellipticals. Systems with L K < 10 10 L ⊙ have lower L X (gas)/SFR ratios than the other galaxies in our sample, perhaps due to lower gravitational fields or lower metallicities. We see no relation between L X (gas)/SFR and Seyfert activity in this sample, suggesting that feedback from active galactic nuclei is not a major contributor to the hot gas in our sample galaxies.

show abstract

Section: 78±mentioning

confidence: 71%

Diffuse X-Ray-emitting Gas in Major Mergers

Smith

Campbell

Struck

et al. 2018

View full text Add to dashboard Cite

show abstract

“…2c). The two galaxies present similar kinematics suggesting a single entity (Richer et al 2003). At the location of their interaction is a very strong 24 μm source and high levels of infrared emission can be found throughout the whole group (Johnson et al 2007).…”

Section: The Samplementioning

confidence: 85%

Probing the dust properties of galaxies up to submillimetre wavelengths

Galametz¹,

Madden²,

Galliano³

et al. 2009

A&A

200

View full text Add to dashboard Cite

Aims. We study the dust properties of four low metallicity galaxies by modelling their spectral energy distributions. This modelling enables us to constrain the dust properties such as the mass, the temperature or the composition to characterise the global ISM properties in dwarf galaxies. Methods. We present 870 μm images of four low metallicity galaxies (NGC 1705, Haro 11, Mrk 1089 and UM 311) observed with the Large APEX BOlometer CAmera (LABOCA) on the Atacama Pathfinder EXperiment (APEX) telescope. We modeled their spectral energy distributions combining the submm observations of LABOCA, 2MASS, IRAS, Spitzer photometric data, and the IRS data for Haro 11. Results. We found that the PAH mass abundance is very low in these galaxies, 5 to 50 times lower than the PAH mass fraction of our Galaxy. We also found that a significant mass of dust is revealed when using submm constraints compared to that measured with only mid-IR to far-IR observations extending only to 160 μm. For NGC 1705 and Haro 11, an excess in submillimeter wavelengths was detected when we used our standard dust SED model. We rerun our SED procedure adding a cold dust component (10 K) to better describe the high 870 μm flux derived from LABOCA observations, which significantly improves the fit. We found that at least 70% of the dust mass of these two galaxies can reside in a cold dust component. We also showed that the subsequent dust-to-gas mass ratios, considering HI and CO observations, can be strikingly high for Haro 11 in comparison with what is usually expected for these low-metallicity environments. Furthermore, we derived the star formation rate of our galaxies and compared them to the Schmidt law. Haro 11 falls anomalously far from the Schmidt relation. These results may suggest that a reservoir of hidden gas could be present in molecular form not traced by the current CO observations. While there can be a significant cold dust mass found in Haro 11, the SED peaks at exceptionally short wavelengths (36 μm), also highlighting the importance of the much warmer dust component heated by the massive star clusters in Haro 11. We also derived the total IR luminosities derived from our models and compared them with relations that derive this luminosity from Spitzer bands. We found that the Draine & Li (2007) formula compares well to our direct IR determinations.

show abstract

“…Figure 2 shows the velocity gradients of the objects A1, A2, E, and F, situated around the pair AϩC (see Fig. 1, top right) and which have been thought to be candidate tidal dwarf galaxies (Hunsberger et al 1996, Iglesias-Páramo & Vílchez 2001, and Richer et al 2003. The curves are not corrected for inclination, and the central position and velocity were chosen such that the curves were as symmetric as possible, with both sides matching when possible.…”

Section: Resultsmentioning

confidence: 99%

“…The best candidates are objects E and F, for which metallicities were measured, and they were determined to be similar to that of the complex AϩC, suggesting a tidal origin for these objects (Richer et al 2003).…”

Section: Tidal Fragmentsmentioning

confidence: 99%

“…The spectral resolution of our maps is nevertheless 6 times higher (7900 vs. 45,900) and the detection limit several magnitudes fainter. Several authors supported that A and C are separate entities in an ongoing merging phase (e.g., Vorontsov-Velyaminov & Arkhipova 1963; Rubin et al 1990), while Richer et al (2003) supported the scenario that AϩC is a single interacting spiral galaxy. The new piece of evidence in support of the merging scenario reported in this Letter is the presence of double velocity components throughout the system AϩC.…”

mentioning

confidence: 99%

See 1 more Smart Citation

The Compact Group of Galaxies HCG 31 in an Early Phase of Merging

Amram

Oliveira

Plana

et al. 2004

ApJ

View full text Add to dashboard Cite

We have obtained high spectral resolution ( ) Fabry-Perot velocity maps of the Hickson compact R p 45,900 group HCG 31 in order to revisit the important problem of the merger nature of the central object AϩC and to derive the internal kinematics of the candidate tidal dwarf galaxies in this group. Our main findings are as follows:(1) double kinematic components are present throughout the main body of AϩC, which strongly suggests that this complex is an ongoing merger; (2) regions A2 and E, to the east and south of complex AϩC, present rotation patterns with velocity amplitudes of ∼25 km s Ϫ1 , and they counterrotate with respect to AϩC; and (3) region F, which was previously thought to be the best example of a tidal dwarf galaxy in HCG 31, presents no rotation and negligible internal velocity dispersion, as is also the case for region A1. HCG 31 presents an undergoing merger in its center (AϩC), and it is likely that it has suffered additional perturbations due to interactions with the nearby galaxies B, G, and Q.

show abstract

Is HCG 31 undergoing a merger or a fly-by interaction?

Cited by 15 publications

References 42 publications

Diffuse X-Ray-emitting Gas in Major Mergers

Diffuse X-Ray-emitting Gas in Major Mergers

Probing the dust properties of galaxies up to submillimetre wavelengths

The Compact Group of Galaxies HCG 31 in an Early Phase of Merging

Contact Info

Product

Resources

About