H i observations of giant low surface brightness galaxies

Matthews, L. D.; Driel, W. van; Monnier-Ragaigne, D.

doi:10.1051/0004-6361:20000002

Cited by 67 publications

(65 citation statements)

References 55 publications

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“…For Malin 1, we obtained S tot = 2.0 ± 0.2 Jy km s −1 , consistent within the errors with the value derived by Pickering et al (1997) (S tot = 2.5 ± 0.2 Jy km s −1 ) and the single-dish measurement by Matthews et al (2001) (S tot = 1.80 ± 0.50 Jy km s −1 ). For A&A 516, A11 (2010) References.…”

Section: H I Data Analysissupporting

confidence: 90%

“…Single-dish observations gave intermediate values, consistent with our value within about 1σ: S tot = 2.96 ± 0.51 Jy km s −1 (Matthews et al 2001) and S tot = 3.07 ± 0.36 Jy km s −1 (Springob et al 2005) (this latter value is without the correction for H I self absorption). H I masses were estimated using the luminosity distance D L , given by:…”

Section: H I Data Analysissupporting

confidence: 90%

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Structure and dynamics of giant low surface brightness galaxies

Lelli

Fraternali

Sancisi

2010

A&A

141

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Giant low surface brightness (GLSB) galaxies are commonly thought to be massive, dark matter dominated systems. However, this conclusion is based on highly uncertain rotation curves. We present here a new study of two prototypical GLSB galaxies: Malin 1 and NGC 7589. We re-analysed existing H I observations and derived new rotation curves, which were used to investigate the distributions of luminous and dark matter in these galaxies. In contrast to previous findings, the rotation curves of both galaxies show a steep rise in the central parts, typical of high surface brightness (HSB) systems. Mass decompositions with a dark matter halo show that baryons may dominate the dynamics of the inner regions. Indeed, a "maximum disk" fit gives stellar mass-to-light ratios in the range of values typically found for HSB galaxies. These results, together with other recent studies, suggest that GLSB galaxies are systems with a double structure: an inner HSB early-type spiral galaxy and an outer extended LSB disk. We also tested the predictions of MOND: the rotation curve of NGC 7589 is reproduced well, whereas Malin 1 represents a challenging test for the theory.

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Section: H I Data Analysissupporting

confidence: 90%

Section: H I Data Analysissupporting

confidence: 90%

Structure and dynamics of giant low surface brightness galaxies

Lelli

Fraternali

Sancisi

2010

A&A

141

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“…It has an effective collecting area of roughly 7000 m 2 (equivalent to a 94 m diameter parabolic dish). Due to the elongated geometry of the mirrors, at 21 cm wavelength it has a half-power beam width (HPBW ) of 3A6 EYW ; 22 0 NYS for declinations below 30 ; at higher declinations the NYS HPBW increases (see plot in Matthews et al 2001). Typical system temperatures were $40 K for our project.…”

Section: Nançay H I Observationsmentioning

confidence: 98%

The Photometric and Kinematic Structure of Face‐on Disk Galaxies. I. Sample Definition, Hα Integral Field Spectroscopy, and H i Line Widths

Andersen¹,

Bershady²,

Sparke³

et al. 2006

ASTROPHYS J SUPPL S

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We present a survey of the photometric and kinematic properties of 39 nearby, nearly face-on disk galaxies. Our approach exploits echelle-resolution integral-field spectroscopy of the H regions, obtained with DensePak on the WIYN 3.5 m telescope Bench Spectrograph. These data are complemented by H i line profiles observed with the Nançay radio telescope for 25 of these sample galaxies. Twelve additional line widths are available for sample galaxies from the literature. In this paper, we introduce the goals of this survey, define the sample selection algorithm, and amass the integral field spectroscopic data and H i line widths. We establish spatially integrated H line widths for the sample. We test the veracity of these spatially integrated line profiles by convolving narrowband imaging data with velocity field information for one of the sample galaxies, PGC 38268, and also by comparing to H i line profiles. We find H i and H line profiles to be similar in width but different in shape, indicating that we are observing different spatial distributions of ionized and neutral gas in largely axisymmetric systems with flat outer rotation curves. We also find vertical velocity dispersions of the ionized disk gas within several disk scale lengths have a median value of 18 km s À1 and an 80% range of 12Y26 km s À1 . This is only a factor of $2 larger than what is observed for neutral atomic and molecular gas. With standard assumptions for intrinsic and thermal broadening for H , this translates into a factor of 3 range in turbulent velocities, between 8 and 25 km s À1 .

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“…Pickering et al 1997;Matthews et al 2001;O'Neil 2002, andO'Neil et al 2004). However, the gas mass converted into stars must be lower in LSBs than in HSBs.…”

Section: 66σ Beyond the Freeman Value)mentioning

confidence: 99%

The large-scale environment of low surface brightness galaxies

Rosenbaum

Krusch

Bomans

et al. 2009

A&A

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Context. The exact formation scenarios and evolutionary processes that led to the existence of the class of low surface brightness galaxies (LSBs) have not yet been understood completely. There is evidence that the lack of star formation expected to be typical of LSBs can only occur if the LSBs were formed in low-density regions. Aims. Since the environment of LSBs has been studied before only on small scales (below 2 Mpc), a study of the galaxy content in the vicinity of LSB galaxies on larger scales could add a lot to our understanding of the origin of this galaxy class. Methods. We used the spectroscopic main galaxy sample of the SDSS DR4 to investigate the environmental galaxy density of LSB galaxies compared to the galaxy density in the vicinity of high surface brightness galaxies (HSBs). To avoid the influence of evolutionary effects depending of redshift and to minimize completeness issues within the SDSS, we limited the environment studies to the local universe with a redshift of z ≤ 0.1. At first we studied the luminosity distribution of the LSB sample obtained from the SDSS within two symmetric redshift intervals (0.01 < z ≤ 0.055 and 0.055 < z ≤ 0.1). Results. It was found that the lower redshift interval is dominated by small, low-luminosity LSBs, whereas the LSB sample in the higher redshift range mainly consists of larger, more luminous LSBs. This comes from selection effects of the SDSS spectroscopic sample. The environment studies, also divided into these two redshift bins, show that both the low mass, and the more massive LSBs possess an environment with a lower galaxy density than HSBs. The differences in the galaxy density between LSBs and HSBs are significant on scales between 2 and 5 Mpc, the scales of groups and filaments. To quantify this, we have introduced for the first time the LSB-HSB Antibias. The obtained LSB-HSB Antibias parameter has a value of 10%-15%. Conclusions. From these results we conclude that LSBs formed in low-density regions of the initial universe and have drifted until now to the outer parts of the filaments and walls of the large-scale structure. Furthermore, our results, together with actual cosmological simulations, show that LSBs are caused by a mixture of nature and nurture.

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H i observations of giant low surface brightness galaxies

Cited by 67 publications

References 55 publications

Structure and dynamics of giant low surface brightness galaxies

Structure and dynamics of giant low surface brightness galaxies

The Photometric and Kinematic Structure of Face‐on Disk Galaxies. I. Sample Definition, Hα Integral Field Spectroscopy, and H i Line Widths

The large-scale environment of low surface brightness galaxies

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