The interstellar extinction law from 1 to 13 microns

Rieke, G. H.; Lebofsky, M. J.

doi:10.1086/162827

Cited by 2,173 publications

(2,633 citation statements)

References 0 publications

Supporting

Mentioning

2,507

Contrasting

Unclassified

Order By: Relevance

“…Comparison of a DUSTY SED with the observed one is made by convolving the model SED with each filter's bandpass. We choose not to deredden the observed SED from the effect of foreground Galactic dust as the amplitude of this correction is negligible from the MIR upward (Rieke & Lebofsky 1985). A χ-square procedure is used to determine the best model.…”

Section: Results From the Modelmentioning

confidence: 99%

The Embedded Super-Star Cluster of SBS 0335-052

Plante

Sauvage

2002

The Evolution of Galaxies

View full text Add to dashboard Cite

We analyze the infrared (6-100 µm) spectral energy distribution of the blue compact dwarf and metal-poor (Z=Z ⊙ /41) galaxy SBS 0335-052. With the help of DUSTY (Ivezić et al. 1999), a program that solves the radiation transfer equations in a spherical environment, we evaluate that the infrared (IR) emission of SBS 0335-052 is produced by an embedded super-star cluster (SSC) hidden under 10 5 M ⊙ of dust, causing 30 mag of visual extinction. This implies that one cannot detect any stellar emission from the 2×10 6 M ⊙ stellar cluster even at nearinfrared (NIR) wavelengths. The derived grain size distribution departs markedly from the widely accepted size distribution inferred for dust in our galaxy (the so-called MRN distribution, Mathis et al. (1977)), but resembles what is seen around AGNs, namely an absence of PAH and smaller grains, and grains that grow to larger sizes (around 1 µm). The fact that a significant amount of dust is present in such a low-metallicity galaxy, hiding from UV and optical view most of the star formation activity in the galaxy, and that the dust size distribution cannot be reproduced by a standard galactic law, should be borne in mind when interpreting the spectrum of primeval galaxies.

show abstract

Section: Results From the Modelmentioning

confidence: 99%

The Embedded Super-Star Cluster of SBS 0335-052

Plante

Sauvage

2002

The Evolution of Galaxies

View full text Add to dashboard Cite

show abstract

“…This is converted into extinction in I band using the relation A(I) = 0.934E(V − I), where E(V−I) is the internal reddening value estimated for each location. The above relation is derived from the relations E(V − I) = 1.6E(B − V ) and A(I) = 0.482A(V ) (Rieke & Lebofsky 1985).…”

Section: Discussionmentioning

confidence: 99%

Line of sight depth of the Large and Small Magellanic Clouds

Subramaniam¹,

Subramaniam²

2008

Proc. IAU

View full text Add to dashboard Cite

Abstract. We used the red clump stars from the Optical Gravitational Lensing Experiment (OGLE II) survey and the Magellanic Cloud Photometric Survey (MCPS), to estimate the line-of-sight depth. The observed dispersion in the magnitude and colour distribution of red clump stars is used to estimate the line-of-sight depth, after correcting for the contribution due to other effects. This dispersion due to depth, has a range from minimum dispersion that can be estimated, to 0.46 mag (a depth of 500 pc to 10.44 kpc), in the LMC. In the case of the SMC, the dispersion ranges from minimum dispersion to 0.35 magnitude (a depth of 665 pc to 9.53 kpc). The thickness profile of the LMC bar indicates that it is flared. The average depth in the bar region is 4.0±1.4 kpc. The halo of the LMC (using RR Lyrae stars) is found to have larger depth compared to the disk/bar, which supports the presence of an inner halo for the LMC. The large depth estimated for the LMC bar and the disk suggests that the LMC might have had minor mergers. In the case of the SMC, the bar depth (4.90±1.23 kpc) and the disk depth (4.23±1.48 kpc) are found to be within the standard deviations. We find evidence for an increase in depth near the optical center (up to 9 kpc). On the other hand, the estimated depth for the halo (RR Lyrae stars) and disk (RC stars) for the bar region of the SMC is found to be similar. Thus, increased depth and enhanced stellar as well as H i density near the optical center suggests that the SMC may have a bulge.

show abstract

“…2). From the known slope of the reddening vector (Rieke & Lebofsky 1985) and the gradient of the line (dotted in Fig. 2) the magnitude of the vector A v can be calculated via simple geometric arguments.…”

Section: Dereddening the Samplementioning

confidence: 99%

“…Therefore in practice, because A v is rather more dependent on J − H than H − K (Fig. 3), we have used the J-magnitude flag A, B or C to determine ∆A v = ±1, 2 or 3 mag, with corresponding ∆I and ∆J from the usual relations (Rieke & Lebofsky 1985), approximated in Fig. 11.…”

Section: Treatment Of Errors In Dereddened Magnitudesmentioning

confidence: 99%

A deep, wide-field search for substellar members in NGC 2264

Kendall

Bouvier

Moraux³

et al. 2005

A&A

View full text Add to dashboard Cite

Abstract.We report the first results of our ongoing campaign to discover the first brown dwarfs (BD) in NGC 2264, a young (3 Myr), populous star forming region for which our optical studies have revealed a very high density of potential candidates -236 in <1 deg 2 -from the substellar limit down to at least ∼20 M Jup for zero reddening. Candidate BD were first selected using wide field (I, z) band imaging with CFH12K, by reference to current theoretical isochrones. Subsequently, 79 (33%) of the I, z sample were found to have near-infrared 2MASS photometry (JHK s ± 0.3 mag or better), yielding dereddened magnitudes and allowing further investigation by comparison with the location of NextGen and DUSTY isochrones in colourcolour and colour-magnitude diagrams involving various combinations of I, J, H and K s . We discuss the status and potential substellarity of a number of relatively unreddened (A v < ∼ 5) likely low-mass members in our sample, but in spite of the depth of our observations in I, z, we are as yet unable to unambiguously identify substellar candidates using only 2MASS data. Nevertheless, there are excellent arguments for considering two faint (observed I ∼ 18.4 and 21.2) objects as cluster candidates with masses respectively at or rather below the hydrogen burning limit. More current candidates could be proven to be cluster members with masses around 0.1 M via gravity-sensitive spectroscopy, and deeper near-infrared imaging will surely reveal a hitherto unknown population of young brown dwarfs in this region, accessible to the next generation of deep near-infrared surveys.

show abstract

The interstellar extinction law from 1 to 13 microns

Cited by 2,173 publications

References 0 publications

The Embedded Super-Star Cluster of SBS 0335-052

The Embedded Super-Star Cluster of SBS 0335-052

Line of sight depth of the Large and Small Magellanic Clouds

A deep, wide-field search for substellar members in NGC 2264

Contact Info

Product

Resources

About