Properties of dust in early-type galaxies

Patil, M. K.; Pandey, S. K.; Sahu, D. K.; Kembhavi, Ajit

doi:10.1051/0004-6361:20053512

Cited by 50 publications

(146 citation statements)

References 41 publications

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“…This confirms the marginal or no detection of the molecular gas in the core of ZwCl 2701. Further, residual image obtained after subtracting a smooth elliptical model of the HST 606 nm optical image (Patil et al 2007;Vagshette et al 2012) could not substantiate the expected signatures of dust features (bottom right panel of Figure 10). Marginal detection of dust and undetectable or very weak MIR/FIR emission from the core of this cluster indicate a very low rate of star formation.…”

Section: Cooling Versus Heating Of the Icmmentioning

confidence: 90%

AGN-driven perturbations in the intracluster medium of the cool-core cluster ZwCl 2701

Vagshette¹,

Sonkamble²,

Naik³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the results obtained from a total of 123 ks X-ray (Chandra) and 8 hrs of 1.4 GHz radio (Giant Metrewave Radio Telescope -GMRT) observations of the cool core cluster ZwCl 2701 (z = 0.214). These observations of ZwCl 2701 showed the presence of an extensive pair of ellipsoidal cavities along the East and West directions within the central region < 20 kpc. Detection of bright rims around the cavities suggested that the radio lobes displaced Xray emitting hot gas forming shell-like structures. The total cavity power (mechanical power) that directly heated the surrounding gas and cooling luminosity of the cluster were estimated to be ∼ 2.27 × 10 45 erg s −1 and 3.5× 10 44 erg s −1 , respectively. Comparable values of cavity power and cooling luminosity of ZwCL 2701 suggested that the mechanical power of the AGN outburst is large enough to balance the radiative cooling in the system. The star formation rate derived from the Hα luminosity was found to be ∼ 0.60 M yr −1 which is about three orders of magnitude lower than the cooling rate of ∼ 196 M yr −1 . Detection of the floor in entropy profile of ZwCl 2701 suggested the presence of an alternative heating mechanism at the centre of the cluster. Lower value of the ratio (∼10 −2 ) between black hole mass accretion rate and Eddington mass accretion rate suggested that launching of jet from the super massive black hole is efficient in ZwCl 2701. However, higher value of ratio (∼10 3 ) between black hole mass accretion rate and Bondi accretion rate indicated that the accretion rate required to create cavities is well above the Bondi accretion rate.

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Section: Cooling Versus Heating Of the Icmmentioning

confidence: 90%

AGN-driven perturbations in the intracluster medium of the cool-core cluster ZwCl 2701

Vagshette¹,

Sonkamble²,

Naik³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Bedregal et al 2006;Davis et al 2011). Nevertheless, many recent works claim that the dust content of S0s may have been significantly underestimated (Patil et al 2007;Riad et al 2010;Rowlands et al 2012;di Serego Alighieri et al 2013) and that an improper dust correction could lead to underestimation of the luminosity of a galaxy (or, equivalently, its stellar mass) to ∼ 40% of its real value (Zibetti et al 2009). …”

Section: Appendix A: Dust Extinctionmentioning

confidence: 99%

Formation of S0 galaxies through mergers

Tapia

Eliche‐Moral

Aceves

et al. 2017

A&A

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Context. Lenticular (S0) galaxies are known to derive from spiral galaxies. The fact that S0s nearly obey the Tully-Fisher relation (TFR) at z ∼ 0 (as spirals have done in the last ∼9 Gyr) is considered an argument against their major-merger origin because equal mergers of two disc galaxies produce remnants that are outliers of the TFR. Aims. We explore whether a scenario that combines an origin by mergers at z ∼ 1.8 − 1.5 with a subsequent passive evolution of the resulting S0 remnants since z ∼ 0.8-1 is compatible with observational data of S0s in the TFR both at z ∼ 0.8 and z ∼ 0. Methods. We studied a set of major and minor merger experiments from the GalMer database that generate massive S0 remnants that are dynamically relaxed and have realistic properties. We analysed the location of these remnants in the photometric and stellar TFRs assuming that they correspond to z ∼ 0.8 galaxies. We then estimated their evolution in these planes over the last ∼ 7 Gyr considering that they have evolved passively in isolation. The results were compared with data of real S0s and spirals at different redshifts. We also tested how the use of V circ or V rot,max affects the results. Results. Just after ∼ 1-2 Gyr of coalescence, major mergers generate S0 remnants that are outliers of the local photometric and stellar TFRs (as already stated in previous studies), in good agreement with observations at z ∼ 0.8. After ∼ 4 -7 Gyr of passive evolution in isolation, the S0 remnants move towards the local TFR, although the initial scatter among them persists. This scatter is sensitive to the indicator used for the rotation velocity: V circ values yield a lower scatter than when V rot,max values are considered instead. In the planes involving V rot,max , a clear segregation of the S0 remnants in terms of the spin-orbit coupling of the model is observed, in which the remnants of retrograde encounters overlap with local S0s hosting counter-rotating discs. The location of the S0 remnants at z ∼ 0 agrees well with the observed distribution of local S0 galaxies in the σ 0 -M K , V circ -σ 0 , and V rot,max -σ 0 planes. Conclusions. Massive S0 galaxies may have been formed through major mergers that occurred at high redshift and have later evolved towards the local TFR through passive evolution in relative isolation, a mechanism that would also contribute to the scatter observed in this relation.

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“…Another novel method of studying extragalactic dust extinction is through the study of early-type galaxies with resolved dust lanes (e.g. Goudfrooij et al 1994;Patil et al 2007;Finkelman et al 2008Finkelman et al , 2010. For those such galaxies with a relatively small dust covering factor, and a spatially smooth underlying stellar light distribution, the spectra of the underlying, dust-free galaxy can be measured with reasonable accuracy.…”

Section: Introductionmentioning

confidence: 99%

The dust extinction curves of gamma-ray burst host galaxies

Schady¹,

Dwelly²,

Page³

et al. 2011

A&A

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The composition and amount of interstellar dust within gamma-ray burst (GRB) host galaxies is of key importance when addressing selection effects in the GRB redshift distribution, and when studying the properties of their host galaxies. As well as the implications for GRB research, probing the dust within the high-z hosts of GRBs also contributes to our understanding of the conditions of the interstellar medium and star-formation in the distant Universe. Nevertheless, the physical properties of dust within GRB host galaxies continues to be a highly contended issue. In this paper we explore the mean extinction properties of dust within the host galaxies of a sample of 17 GRBs with total host galaxy visual extinction A V < 1 ( A V = 0.4), covering a redshift range z = 0.7−3.1. We find the average host extinction curve to have an ultraviolet slope comparable to that of the LMC, but with little evidence of a 2175 Å dust extinction feature as observed along Milky Way and LMC sightlines. We cannot at present rule out the presence of a 2175 Å feature, and both the standard SMC and LMC extinction curves also provide good fits to our data. However, we can reject an extinction curve that has a UV slope as flat as the mean Milky Way extinction curve, whilst also having a 2175 Å feature as prominent as seen in the mean Milky Way extinction curve. This is in contrast to the clear detection of a 2175 Å bump and the flatter extinction curves of some more heavily extinguished GRBs (A V > 1), which may be indicative of there being a dependence between dust abundance and the wavelength dependence of dust extinction, as has been previously speculated.

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Properties of dust in early-type galaxies

Cited by 50 publications

References 41 publications

AGN-driven perturbations in the intracluster medium of the cool-core cluster ZwCl 2701

AGN-driven perturbations in the intracluster medium of the cool-core cluster ZwCl 2701

Formation of S0 galaxies through mergers

The dust extinction curves of gamma-ray burst host galaxies

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