The mass-to-light ratios of low surface brightness spiral galaxies: Clues from the Tully-Fisher relation

Sprayberry, David; Bernstein, G. M.; Impey, C. D.; Bothun, G. D.

doi:10.1086/175055

Cited by 89 publications

(99 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Even though many groups have been working on this subject, there is still no agreement as to whether there exists any fine-tuning between central surface brightness and the total mass-to-light ratio that makes disk galaxies follow the TF relation. For instance, Zwaan et al (1995) and Sprayberry et al (1995a) find that the LSB galaxies follow the same TF relation defined by normal spiral, while Persic & Salucci (1991) and Matthews et al (1998b) find a curvature (underluminous at a given line width) at the low-luminosity end of the TF relation for LSB galaxies.…”

Section: Discussionmentioning

confidence: 97%

“…As Matthews et al (1998b) point out, the star formation history and evolutionary states of LSB galaxies studied using the TF relation give different interpretations strongly depending on the sample galaxies. For example, investigators who studied galaxies comparable to or larger than normal-size galaxies conclude that LSB galaxies do follow the same TF relation (Zwaan et al 1995;Sprayberry et al 1995a), while others, who included smaller LSBs, find larger scatter in the TF relation (Matthews et al 1998b). Here we have a good sample (O'Neil et al 1997a), which is diverse in terms of sizes and colors, and, in fact, we see a larger scatter even if we exclude the contaminated LSBs.…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Low Surface Brightness Galaxies and the Tully-Fisher Relation

Chung

Gorkom

O'Neil

et al. 2002

The Astronomical Journal

Self Cite

View full text Add to dashboard Cite

We present Very Large Array (VLA) H i imaging of four low surface brightness (LSB) galaxies ([OBC97] P01-3, [OBC97] C06-1, [OBC97] C04-1, [OBC97] C04-2), 1 which were thought to strongly deviate from the Tully-Fisher (TF) relation based on Arecibo single-dish observations. We do not detect three of the four targeted low surface brightness galaxies (LSBs) in H i down to a 4 limit of 0.08 Jy km s À1 . We find that two of the four of these LSBs have bright galaxies at projected distances of 2<6 and 2<9, which have contaminated the Arecibo signal. A further examination of the Arecibo sample shows that five out of the six galaxies that were found to deviate from the TF relation have nearby bright galaxies (within 3<5 and within the observed H i velocity range), and we conclude that possibly all but one of the non-TF galaxies are contaminated by H i from nearby galaxies. The sixth galaxy was not detected by us. A new observation by Arecibo did not confirm the earlier detection. We present the H i properties, kinematics, and rotation curves of three bright galaxies NGC 7631, KUG 2318+078, NGC 2595 which happened to be in the LSB fields and of two LSB galaxies, one of the targeted ones C04-2 and one (UGC 12535 or P01-1) that was found in the field of P01-3. The two detected LSB galaxies fall within 2 on the TF relation. The integrated profiles of the bright galaxies are consistent with the Arecibo results both in velocity range and amplitude, which indicates that most of the extreme deviators from the TF relation must have been affected by bright companions in this earlier H i survey. A more recent determination of the sidelobe structure of the Arecibo beam supports our conclusion and shows that the degree of sidelobe contamination was much larger than could have been initially predicted. If the now unknown velocities of these nondetected LSB's are within our probed velocity range then the limit to their H i mass is roughly 10 8 M assuming H 0 = 75 km s À1 Mpc À1 . Hence, we have corrected the results found in O'Neil et al. (2000a) and have reconstructed the TF relation. These new observations then show (1) a reconstructed TF relation that has relatively large scatter at all values of rotational velocity (possibly indicating the true range in disk galaxy properties) and (2) the presence of at least some red, gas-poor, LSB disks that indeed may be in an advanced evolutionary state as the faded remnants of their former high surface brightness actively star-forming state.

show abstract

Section: Discussionmentioning

confidence: 97%

Section: Discussionmentioning

confidence: 99%

Low Surface Brightness Galaxies and the Tully-Fisher Relation

Chung

Gorkom

O'Neil

et al. 2002

The Astronomical Journal

Self Cite

View full text Add to dashboard Cite

show abstract

“…For example, estimates of dust reddening, even if small, are needed to correctly interpret the stellar populations inferred from broadband colors and spectroscopic measurements (e.g., Bell et al 2000). It has been found that many of the lowest luminosity LSB galaxies deviate from the standard optical Tully-Fisher relation in the sense that they rotate faster than predicted for their luminosities (e.g., Matthews, van Driel, & Gallagher 1998 ;Stil 1999 ;McGaugh et al 2000), while more luminous LSB galaxies seem to follow the same Tully-Fisher relation as higher surface brightness galaxies (e.g., Zwaan et al 1995 ;Sprayberry et al 1995). This appears to have important implications for galaxy formation models (e.g., van den Bosch 2000) and for establishing the possible existence of a "" baryonic ÏÏ Tully-Fisher relation (e.g., Matthews et al 1998 ;McGaugh et al 2000) ; however, the internal extinction corrections appropriate for the LSB galaxies used in these analyses remains a point of contention (e.g., Han 1992 ;Rhee 1996 ;Matthews et al 1998 ;Pierni 1999).…”

mentioning

confidence: 97%

Modeling the Interstellar Medium of Low Surface Brightness Galaxies: Constraining Internal Extinction, Disk Color Gradients, and Intrinsic Rotation Curve Shapes

Matthews

Wood

2001

Astrophysical Journal

View full text Add to dashboard Cite

We use a combination of three-dimensional Monte Carlo radiative transfer techniques and multiwavelength (BRHK, Ha) imaging data to investigate the nature of the interstellar medium (ISM) in the edge-on, low surface brightness (LSB) galaxy UGC 7321. Using realistic models that incorporate multiple scattering e †ects and clumping of the stars and the interstellar material, we explore the distribution and opacity of the interstellar material (gas]dust) and its e †ects on the observed stellar disk luminosity proÐles, color gradients, and rotation curve shape. We Ðnd that UGC 7321 contains a small but nonnegligible dusty component to its ISM, yielding a B-band optical depth from disk edge to q6 e,B D 4.0 center. A signiÐcant fraction (D50%^10%) of the interstellar material in the innermost regions of UGC 7321 appears to be contained in a clumpy medium, indicating that LSB galaxies can support a modest, multiphase ISM structure. In spite of the clear presence of dust, we conclude that the large radial optical color gradients observed in UGC 7321 and other similar LSB spiral galaxies cannot be accounted for by dust and must result primarily from signiÐcant stellar population and/or metallicity gradients. We show that realistic optical depth e †ects will have little impact on the observed rotation curves of edge-on disk galaxies and cannot explain the linear, slowly rising rotation curves seen in some edge-on LSB spirals. Projection e †ects create a far larger uncertainty in recovering the true underlying rotation curve shape of galaxies viewed at inclinations i Z 85¡.

show abstract

“…For all HSB galaxies, the combination of this relation and the virial theorem yields μ HSB πk 2 M b = V 4 , and the TFR can be understood as a constant baryon-to-total mass ratio. When another category of galaxies of low surface brightness (LSB) were discovered, violating Freeman's relation (Sprayberry et al 1995), it was found that they also satisfied the same TFR, i.e. μ LSB πk 2 LSB M b = V 4 , or in other words that μk 2 was an invariant for all categories.…”

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

“…It could help for understanding galaxy evolution along the Hubble sequence, bars in galaxies, low-surface-brightness objects, or luminosity evolution (Burstein 1982;Sprayberry et al 1995;Zwaan et al 1995;Barton et al 2001;Courteau et al 2003). This type of work from scaling physical relations was developed in parallel for elliptical galaxies, which are more difficult to deproject, and deep development beyond the Faber-Jackson relation were worked out towards the fundamental plane (Djorgovski et al 1987).…”

mentioning

confidence: 99%

From distances to galaxy evolution and the dark matter problem

Combes¹

2009

A&A

View full text Add to dashboard Cite

Thirty-two years ago, Brent Tully and Richard Fisher wrote this ground-breaking article on a method of determining galaxy distances that is independent of redshift. This method is now the most widely used one for spiral galaxies. They proposed using a correlation between a distance-independent observable for spiral galaxies, the global neutral atomic hydrogen (HI) profile width, and their absolute magnitude or global luminosity, to indicate distances. It was not the first time that comparable correlations were used as distance indicators (e.g. Roberts 1962;Balkowski et al. 1973;Shostak 1974), and the virial theorem was invoked as the basis. But the simple correlation between luminosity and rotational velocity had not yet been approached. Also many other correlations had been studied, such as a correlation with morphological type, so that the breakthrough in this paper was to show that the correlation with type was secondary (since early type objects are more massive and luminous) and that the principal and original correlation was with luminosity.As The difficulty of convincing the community of the quality of the correlation was to reduce the errors that flawed early attempts to calibrate it: by more accurately knowing the distance of nearby galaxies, their inclination corrections of the intrinsic rotational velocity, and corrections to magnitude. Tully and Fisher succeeded in obtaining good calibrators with careful corrections, and then applied the relation to finding the distance to the Virgo and Ursa Major cluster. They also derived an estimate of the Hubble constant, H 0 = 80 km s −1 Mpc −1 , not so far from the accepted value today (Sakai et al. 2000).The distance to Virgo that they determined (13.2 Mpc) was inconsistent with previous determinations of 19.5 Mpc (Sandage & Tammann 1974), and they argued that the reason was the previous inclusion of the Virgo II southern extension, which does not belong to the same cluster. An interesting feature of their work is that they proposed both the correlation of the HI line width with the magnitude and the diameter of spiral galaxies. Given the uncertainties and the difficulty defining diameters precisely, only the total luminosity was retained in later literature.Although their correlation could also help for understanding galactic structure, Tully & Fisher (1977) put the emphasis on discovering a new method of determining distances, in competition with other distance indicators used as standard candles (peculiar stars or giant HII regions). The correlation turned out to be an impressive tool for distinguishing peculiar motions from expansion and mapping the large-scale structure of the local universe (Dekel 1994). At the beginning, most citations of the 1977 paper were coming from individual galaxy studies, then, and more and more from the large-scale structures and the expansion rate of super-clusters. It was soon realized that the red or infrared magnitudes were much better correlated to the HI line width than the visible one (Aaronson et al. 1979;Giovanelli et ...

show abstract

The mass-to-light ratios of low surface brightness spiral galaxies: Clues from the Tully-Fisher relation

Cited by 89 publications

References 0 publications

Low Surface Brightness Galaxies and the Tully-Fisher Relation

Low Surface Brightness Galaxies and the Tully-Fisher Relation

Modeling the Interstellar Medium of Low Surface Brightness Galaxies: Constraining Internal Extinction, Disk Color Gradients, and Intrinsic Rotation Curve Shapes

From distances to galaxy evolution and the dark matter problem

Contact Info

Product

Resources

About