A Catalog of Neighboring Galaxies

Караченцев, И. Д.; Караченцева, В. Е.; Huchtmeier, W. K.; Макаров, Д. И.

doi:10.1086/382905

Cited by 750 publications

(1,051 citation statements)

References 154 publications

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“…In order to estimate this, we use the catalog of nearby galaxies given by Karachentsev et al (2004). This catalog is nearly complete out to a distance of 10 Mpc and it contains a total of 431 galaxies with known mass for 313 galaxies.…”

Section: Estimation Of the External Fifth Forcementioning

confidence: 99%

Astrophysical tests of modified gravity: the morphology and kinematics of dwarf galaxies

Vikram

Cabré

Jain

et al. 2013

J. Cosmol. Astropart. Phys.

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This paper is the third in a series on tests of gravity using observations of stars and nearby dwarf galaxies. We carry out four distinct tests using published data on the kinematics and morphology of dwarf galaxies, motivated by the theoretical work of Hui et al. (2009) andJain &Vanderplas (2011). In a wide class of gravity theories a scalar field couples to matter and provides an attractive fifth force. Due to their different self-gravity, stars and gas may respond differently to the scalar force leading to several observable deviations from standard gravity. HI gas, red giant stars and main sequence stars can be displaced relative to each other, and the stellar disk can display warps or asymmetric rotation curves aligned with external potential gradients. To distinguish the effects of modified gravity from standard astrophysical phenomena, we use a control sample of galaxies that are expected to be screened from the fifth force. In all cases we find no significant deviation from the null hypothesis of general relativity. The limits obtained from dwarf galaxies are not yet competitive with the limits from cepheids obtained in our first paper, but can be improved to probe regions of parameter space that are inaccessible using other tests. We discuss how our methodology can be applied to new radio and optical observations of nearby galaxies.

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Section: Estimation Of the External Fifth Forcementioning

confidence: 99%

Astrophysical tests of modified gravity: the morphology and kinematics of dwarf galaxies

Vikram

Cabré

Jain

et al. 2013

J. Cosmol. Astropart. Phys.

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“…Hence the question remained how these two types of dwarf galaxies are formed. We have incorporated the above idea in the present model by assuming that the formation of dEs or dIrrs depends on a random variable Θ (Karachentsev et al 2004). We indeed found in an earlier paper (Chattopadhyay et al 2010) that dE galaxy formation is preferred when Θ > 0 and that of dIrrs when Θ < 0.…”

Section: Resultsmentioning

confidence: 99%

“…In a previous paper (Chattopadhyay et al 2010) we classified dwarf galaxies on the basis of several parameters and found two groups, one dominated by dIrrs and the other by dEs, and for these two groups the average value of Θ was negative and positive, respectively. The observed values of Θ, taken from Karachentsev et al(2004), are given in Table 1 along with galaxy names and morphological indices T.…”

Section: Modelmentioning

confidence: 99%

“…The system of equations (6) Karachentsev et al(2004) in Chattopadhyay et al(2010) Galaxy names Θ T Galaxy names Θ T E349-031 0.5 10 UGC7242 0.4 10 E410-005 0.4 -1 DDO113 1.6 10 E294-010 1.0 -3 DDO125 -0.9 10 KDG2 0.4 -1 UGC7605 0.7 10 E540-032 0.6 -3 E381-018 -0.6 10 UGC685 -1.6 9 E443-09 -0.9 10 KKH5 -1.2 10 KK182 1.2 10 KKH6 -0.8 10 UGC8215 -0.5 10 KK16 -0.4 10 E269-58 1.9 10 KK17 -0.3 10 KK189 2.0 -3 KKH34 -0.8 10 E269-66 1.7 -1 E121-20 -1.6 10 KK196 2.2 10 E489-56 -2.1 10 KK197 3.0 -3 KKH37 -0.3 10 KKs55 3.1 -3 UGC3755 -2.1 10 14247 1.5 10 E059-01 -1.5 9 UGC8508 -1.0 10 KK65 -2.0 10 E444-78 2.1 10 UGC4115 -1.7 10 UGC8638 -1.3 10 DDO52 -1.5 10 KKs57 1.8 -3 D564-08 -1.9 10 KK211 1.5 -5 D565-06 -1.8 10 KK213 1.7 -3 KDG61 3.9 -1 KK217 1.1 -3 KKH57 0.7 -3 CenN 0.9 -3 HS117 1.9 10 KKH86 -1.5 10 UGC6541 -0.7 10 UGC8833 -1.4 10 NGC3741 -0.8 10 E384-016 0.3 10 E320-14 -1.2 10 KK230 -1.0 10 KK109 -0.6 10 DDO190 -1.3 10 E379-07 -1.3 10 E223-09 -0.8 10 NGC4163 0.1 10 IC4662 -0.9 9 …”

Section: Appendix 2: Derivation Of Equations 6 To 10mentioning

confidence: 99%

“…This is a more extended version of the galaxy interaction models of Silk & Norman (1981) and Okazaki & Taniguchi (2000). We have considered a random production of dIrr and dE galaxies during each interaction on the basis of an environmental parameter, the tidal index Θ (Karachentsev et al 2004). We describe the model in section 2, the observations are presented in section 3, and the results and interpretations are given in section 4.…”

Section: Introductionmentioning

confidence: 99%

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Formation of dwarf ellipticals and dwarf irregular galaxies by interaction of giant galaxies under environmental influence

et al. 2015

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A model is proposed for the formation of gas-rich dwarf irregular galaxies and gas-poor, rotating dwarf elliptical galaxies following the interaction between two giant galaxies as a function of space density. The formation of dwarf galaxies is considered to depend on a random variable, the tidal index Θ, an environmental parameter defined by Karachentsev et al. (2004), such that for Θ < 0 the formation of dwarf irregular galaxy is assured whereas for Θ > 0 the formation of dwarf ellipticals is preferred. It is found that for particular ranges of the interactive parameters the model predictions are in good agreement with the observed number density of the different galaxy types as a function of space density in four clusters of galaxies. This supports the fact that galaxy interactions do not all necessarily give rise to the formation of either dwarf irregulars or dwarf ellipticals. It is also shown that the formation of dwarf irregulars at high densities is much lower than that of dwarf ellipticals, and that the formation of the latter reaches a maximum at a particular space density, unlike the former. ThisEmail addresses: tanuka@iucaa.ernet.in (Tanuka Chattopadhyay), debsarma@rediffmail.com (Suma Debsarma), edavoust@irap.omp.eu (Emmanuel Davoust)Preprint submitted to Nuclear Physics B March 1, 2018 suggests that at high densities many dwarf irregulars are stripped of their gaseous envelopes to become dwarf elliptical.

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Edge‐on disk galaxies in the SDSS DR6: Fractions of bulgeless and other disk galaxies

Kautsch¹

2009

Astron Nachr

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The aim of this study is to determine the fractions of different spiral galaxy types, especially bulgeless disks, from a complete and homogeneous sample of 15 127 edge-on disk galaxies extracted from the sixth data release from the Sloan Digital Sky Survey. The sample is divided in broad morphological classes and sub types consisting of galaxies with bulges, intermediate types and galaxies which appear bulgeless. A small fraction of disky irregulars is also detected. The morphological separation is based on automated classification criteria which resemble the bulge sizes and the flatness of the disks. Each of these broad classes contains about 1/3 of the total sample. Using strict criteria for selecting pure bulgeless galaxies leads to a fraction of 15% of simple disk galaxies. We compare this fraction to other galaxy catalogs and find an excellent agreement of the observed frequency of bulgeless galaxies. Although the fraction of simple disk galaxies in this study does not represent a "cosmic" fraction of bulgeless galaxies, it shows that the relative abundance of pure disks is comparable to other studies and offers a profound value of the frequency of simple disks in the local Universe. This fraction of simple disks emphasizes the challenge for formation and evolution models of disk galaxies since these models are hard pressed to explain the observed frequency of these objects.

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A Catalog of Neighboring Galaxies

Cited by 750 publications

References 154 publications

Astrophysical tests of modified gravity: the morphology and kinematics of dwarf galaxies

Astrophysical tests of modified gravity: the morphology and kinematics of dwarf galaxies

Formation of dwarf ellipticals and dwarf irregular galaxies by interaction of giant galaxies under environmental influence

Edge‐on disk galaxies in the SDSS DR6: Fractions of bulgeless and other disk galaxies

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