Radially truncated galactic discs

Grijs, Richard de; Kregel, M.; Wesson, Karen H.

doi:10.1046/j.1365-8711.2001.04380.x

Cited by 70 publications

(84 citation statements)

References 32 publications

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“…A similar result was obtained by Moth & Elston (2002) for the HDF North field. As suggested in Tamm & Tenjes (2005), the more curved profiles might indicate the effect known as disk truncation, discovered by studies of local edge-on disk galaxies (de Grijs et al 2001;Pohlen et al 2002) and more recently detected also at higher redshifts (Pérez 2004;Trujillo & Pohlen 2005). Such a luminosity distribution is sometimes fitted by a double-exponential profile (Pohlen et al 2002;Pérez 2004).…”

Section: The Shape Of the Luminosity Profilesmentioning

confidence: 82%

Surface photometry and structure of high redshift disk galaxies in the HDF-S NICMOS field

Tamm

Tenjes

2006

A&A

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Aims. We report on a photometric study of a sample of 22 disk galaxies in the Hubble Deep Field South NICMOS parallel field. The redshift range of the galaxies is z = 0.5−2.6. Methods. We use deep NICMOS J and H band and STIS open mode images, taken as part of the HDF-S project, to construct rest-frame B-profiles and (U − V) color profiles of the galaxies. Before fitting isophotes, images are deconvolved with PSF. Derived surface brightness profiles are approximated by Sérsic luminosity distribution. Results. Significantly large population of disks cannot be represented by an exponential disk, but this can be well done by Sérsic law, if n < 1. This might be the same phenomenon which has earlier been referred to as truncation of disks. Parameter n does not vary significantly with redshift. Galactic sizes decrease with redshift as r e (z)/r e (0) = 1 − 0.26z. The rest frame (U − V) color shows a clear decrease at z ≈ 2, concordantly with the understanding of more intense star formation at earlier epochs. Color gradients ∆(U − V)/∆r are small and roughly constant at z < 2. At z > 2, dominantly positive gradients appear, possibly indicating centrally concentrated star-formation. On the basis of (U − V) color and chemical evolution models, the disks observed at z ∼ 2.5 have formed between z = 3.5−7. Scale radii r e of the galaxies correlate with the scale surface brightnesses µ e for the sample. None of the studied parameters shows clear dependence on absolute B luminosity for the galaxies.

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Section: The Shape Of the Luminosity Profilesmentioning

confidence: 82%

Surface photometry and structure of high redshift disk galaxies in the HDF-S NICMOS field

Tamm

Tenjes

2006

A&A

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“…The reason is twofold: one, stars far from the solar region require the investment of significant observing time; and two, as one approaches the edge of the Galaxy (R G ≈ 16 kpc or d ≈ 8 kpc from the Sun toward l = 180 • ) the stellar density decreases. The galactic stellar scale length is of order 3 kpc for the Milky Way (Zheng et al 2001;López-Corredoira et al 2002) which implies a stellar disk of about 12 kpc based on external spirals (de Grijs et al 2001). López-Corredoira et al however find no indication of a cut-off in the galactic stellar disk at radii R G < 15 kpc.…”

Section: [Fe/h] Distributionmentioning

confidence: 96%

THE DISTRIBUTION OF THE ELEMENTS IN THE GALACTIC DISK. III. A RECONSIDERATION OF CEPHEIDS FROMl= 30° TO 250°

Luck

Lambert

2011

The Astronomical Journal

221

267

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This paper reports on the spectroscopic investigation of 238 Cepheids in the northern sky. Of these stars, about 150 are new to the study of the galactic abundance gradient. These new Cepheids bring the total number of Cepheids involved in abundance distribution studies to over 400. In this work, we also consider systematics between various studies and also those which result from the choice of models. We find that systematic variations exist at the 0.06 dex level both between studies and model atmospheres. In order to control the systematic effects our final gradients depend only on abundances derived herein. A simple linear fit to the Cepheid data from 398 stars yields a gradient d[Fe/H]/dR G = −0.062 ± 0.002 dex kpc −1 which is in good agreement with previously determined values. We have also re-examined the region of the "metallicity island" of Luck et al. With the doubling of the sample in that region and our internally consistent abundances, we find that there is scant evidence for a distinct island. We also find in our sample the first reported Cepheid (V1033 Cyg) with a pronounced Li feature. The Li abundance is consistent with the star being on its redward pass toward the first giant branch.

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“…This effect was later also observed in many galaxies by a number of observational groups, both in edge-on galaxies (Jensen & Thuan 1982;Sasaki 1987;Fry et al 1999;Barteldrees & Dettmar 1994;Pohlen et al 2000a;de Grijs et al 2001;Kregel et al 2002), and also in face-on galaxies (Pompei & Natali 1997;Pohlen et al 2002). For a recent summary of this topic, see van der Kruit (2001).…”

Section: Introductionmentioning

confidence: 64%

“…However, this Letter to the Editor need not be true for all galaxies. Second, it has been argued that if R max arises due to errors in sky subtraction then we should see a similar cut-off in other luminosity distributions like the vertical profiles of disks, which is not seen (de Grijs et al 2001;Barteldrees & Dettmar 1994). Note, however, that the intensity falls much faster along the z-axis than along R-axis for a thin galactic disk.…”

Section: Alternative Solutions and Implicationsmentioning

confidence: 82%

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The puzzle about the radial cut-off in galactic disks

Narayan¹,

Jog²

2003

A&A

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Abstract. The stellar disk in a spiral galaxy is believed to be truncated physically because the disk surface brightness is observed to fall faster than that for an exponential in the outer, faint regions. We review the literature associated with this phenomenon and find that a number of recent observations contradict the truncation picture. Hence we question the very existence of a physical outer cut-off in stellar disks. We show, in this paper, that the observed drop in the surface brightness profiles in fact corresponds to a negligible decrease in intensity, and that this minor change at the faint end appears to be exaggerated on a log-normal plot. Since minor deviations from a perfect exponential are common throughout the disk, we suggest that such a deviation at the faint end could easily give rise to the observed sharp drop.

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Radially truncated galactic discs

Cited by 70 publications

References 32 publications

Surface photometry and structure of high redshift disk galaxies in the HDF-S NICMOS field

Surface photometry and structure of high redshift disk galaxies in the HDF-S NICMOS field

THE DISTRIBUTION OF THE ELEMENTS IN THE GALACTIC DISK. III. A RECONSIDERATION OF CEPHEIDS FROMl= 30° TO 250°

The puzzle about the radial cut-off in galactic disks

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