Malmquist Bias and Virgocentric Model in Tully-Fisher Relation

Bottinelli, L.; Fouqué, P.; Gouguenheim, L.; Paturel, G.; Teerikorpi, P.

doi:10.1007/978-94-009-4702-3_13

Cited by 58 publications

(80 citation statements)

References 6 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The total HI mass of NGC 4004 is determined as 7.2 · 10 9 M . This is in good agreement with the single-dish observations of Davis & Seaquist (1983) (6.15 · 10 9 M ), Gavazzi (1987) (5.77·10 9 M ) and Bottinelli et al (1990) (9.0·10 9 M ) and is a good indicator that we do not miss any faint and extended flux. We estimate an HI mass of the southern tail of 2.6 · 10 9 M , which is 36% of the total HI mass.…”

Section: Ngc 4004supporting

confidence: 92%

“…But considering the starbursting nature of this galaxy, the high velocity dispersion might also be at least partly induced by turbulences within the ISM due to superwinds coming from supernova explosions. Our derived HI mass of 4.3 · 10 9 M is accordance with what is found by Bottinelli et al (1990) (5.57 · 10 9 M ) and Mirabel & Sanders (1988) (5.19 · 10 9 M ). The tidal HI features to the north-west have an approximate mass of ∼ 1.4 · 10 9 M , which is 33% of the total HI gas mass.…”

Section: Arp 161supporting

confidence: 91%

See 1 more Smart Citation

The Structure and Interaction History of Moderate Luminosity Mergers

Hüttemeister¹,

Manthey²

2006

Proc. IAU

View full text Add to dashboard Cite

Interaction and merging are the two most important driving forces of galaxy evolution. In contrast to the well studied major mergers of two large gas-rich disk galaxies, which may lead to Ultraluminous Infrared Galaxies (ULIRGs, LFIR>1012 L⊙), mergers between galaxies of unequal mass or a spiral and an elliptical (S+E mergers) are still poorly understood. These moderate luminosity mergers typically have LFIR > 1011 L⊙. Here, we present the results of our multiwavelength study of a sample of such kind of mergers, including interferometric HI and single-dish CO observations, optical and near-infrared imaging as well as optical spectroscopy.

show abstract

Section: Ngc 4004supporting

confidence: 92%

Section: Arp 161supporting

confidence: 91%

The Structure and Interaction History of Moderate Luminosity Mergers

Hüttemeister¹,

Manthey²

2006

Proc. IAU

View full text Add to dashboard Cite

show abstract

“…This research has made use of the NASA/IPAC extragalactic database (NED), which is operated by the Jet Propul- Bottinelli et al (1990) and Theureau et al (1998) samples, the line width at 20% and 50% of the peak flux, W50 and W20, were provided, though not for all galaxies. In cases where only W20 was available, a conversion to W50 was made from a linear least-squares fit between these two quantities derived from those for galaxies for which both measurements were available.…”

Section: Discussionmentioning

confidence: 99%

“…For the Bottinelli et al (1990) Haynes et al (1999) give a different measure of the line width denoted W21 and defined as the full width between the velocity channels at the 50% level of each horn. We can convert the Haynes et al (1999) W21 to the Bottinelli et al (1990) Bottinelli et al (1990) W50s for galaxies in common reveals little difference, and we assume here that V max -values for the LSBs also map directly into W50.…”

Section: Discussionmentioning

confidence: 99%

Structure of Disk‐dominated Galaxies. II. Color Gradients and Stellar Population Models

MacArthur

Courteau

Bell

et al. 2004

ASTROPHYS J SUPPL S

209

260

View full text Add to dashboard Cite

We investigate optical and near-IR color gradients in a sample of 172 low-inclination galaxies spanning Hubble types S0-Irr. The colors are compared with stellar population synthesis models from which luminosityweighted average ages and metallicities are determined. We explore the effects of different underlying star formation histories and additional bursts of star formation. Our results are robust in a relative sense under the assumption that our galaxies shared a similar underlying star formation history and that no bursts involving more than $10% of the galaxy mass have occurred in the past 1-2 Gyr. Because the observed gradients show radial structure, we measure ''inner'' and ''outer'' disk age and metallicity gradients. Trends in age and metallicity and their gradients are explored as a function of Hubble type, rotational velocity, total near-IR galaxy magnitude, central surface brightness, and scale length. We find strong correlations in age and metallicity with Hubble type, rotational velocity, total magnitude, and central surface brightness in the sense that earlier-type, faster rotating, more luminous, and higher surface brightness galaxies are older and more metal-rich, suggesting an early and more rapid star formation history for these galaxies. The increasing trends with rotational velocity and total magnitude level off for V rot k120 km s À1 and M K P À23 mag, respectively. This effect is stronger for metallicity (than age), which could reflect a threshold potential above which all metals are retained and thus metallicity saturates at the yield. Outer disk gradients are found to be weaker than the inner gradients as expected for a slower variation of the potential and surface brightness in the outer parts. We find that stronger age gradients are associated with weaker metallicity gradients. Trends in gradients with galaxy parameters are compared with model predictions: these trends do not agree with predictions of semianalytic models of hierarchical galaxy formation, possibly owing to the effect of bar-induced radial flows. The observed trends are in agreement with chemo-spectrophotometric models of spiral galaxy evolution based on CDM-motivated scaling laws but none of the hierarchical merging characteristics, implying a strong dependence of the star formation history of spiral galaxies on the galaxy potential and halo spin parameter.

show abstract

“…The locations of the two peak intensities were estimated separately using Gaussian fits to the pro-files. Bottinelli et al (1990) derived an empirical relation to correct for the instrumental broadening. They convolved the H i profile progressively with coarser velocity resolutions for a model galaxy, and determined the broadening.…”

Section: H I Line-widthmentioning

confidence: 99%

GMRTHI observations of the Eridanus group of galaxies

Omar

Dwarakanath

2005

J Astrophys Astron

View full text Add to dashboard Cite

Abstract.The GMRT H i 21cm-line observations of galaxies in the Eridanus group are presented. The Eridanus group, at a distance of ∼ 23 Mpc, is a loose group of ∼ 200 galaxies. The group extends more than 10 Mpc in projection. The velocity dispersion of the galaxies in the group is ∼ 240 km s −1 . The galaxies are clustered into different sub-groups. The overall population mix of the group is 30% (E+S0) and 70% (Sp+Irr). The observations of 57 Eridanus galaxies were carried out with the GMRT for ∼ 200 hour. H i emission was detected from 31 galaxies. The channel rms of ∼ 1 mJy beam −1 was achieved for most of the image-cubes made with 4 hour of data. The corresponding H i column density sensitivity (3σ) is ∼ 1 × 10 20 cm −2 for a velocity-width of ∼ 13.4 km s −1 . The 3σ detection limit of H i mass is ∼ 1.2 × 10 7 M ⊙ for a line-width of 50 km s −1 . Total H i images, H i velocity fields, global H i line profiles, H i mass surface densities, H i disk parameters and H i rotation curves are presented. The velocity fields are analysed separately for the approaching and the receding sides of the galaxies. This data will be used to study the H i and the radio continuum properties, the Tully-Fisher relations, the dark matter halos, and the kinematical and H i lopsidedness in galaxies.

show abstract

Malmquist Bias and Virgocentric Model in Tully-Fisher Relation

Cited by 58 publications

References 6 publications

The Structure and Interaction History of Moderate Luminosity Mergers

The Structure and Interaction History of Moderate Luminosity Mergers

Structure of Disk‐dominated Galaxies. II. Color Gradients and Stellar Population Models

GMRTHI observations of the Eridanus group of galaxies

Contact Info

Product

Resources

About