The Wavelength Dependence of Interstellar Extinction from 1.25 to 8.0 μm Using GLIMPSE Data

By R. Indebetouw, J. Mathis, B. Babler, M. Meade, C. Watson, B. Whitney, Michael J. Wolff, M. Wolfire, M. Cohen, T. Bania and 10 more. 2004

663 citations recorded by the source corpus.

We determine and tabulate A[λ]/AK, the wavelength dependence of interstellar extinction, in the Galactic plane for 1.25 μm ≤ λ ≤ 8.0 μm along two lines of sight: l = 42° and 284°. The first is a relatively quiescent and unremarkable region; the second contains the giant H II region RCW 49, as well as a "field" region unrelated to the cluster and nebulosity. Areas near these Galactic longitudes were imaged at J, H, and K bands by 2MASS and at 3-8 μm by Spitzer for the GLIMPSE Legacy program. We measure the mean values of the color excess ratios (A[λ] - AK)/(AJ - AK) directly from the color distributions of observed stars. The extinction ratio between two of the filters, e.g., AJ/AK, is required to calculate A[λ]/AK from those measured ratios. We use the apparent JHK magnitudes of giant stars along our two sight lines and fit the reddening as a function of magnitude (distance) to determine AJ kpc-1, AK kpc-1, and AJ/AK. Our values of A[λ]/AK show a flattening across the 3-8 μm wavelength range, roughly consistent with the extinction measurements derived by Lutz and coworkers for the sight line toward the Galactic center.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

2MASS wide field extinction maps. I. The Pipe nebula (2006, methodology): “We found as best fit slope α = 1.82 ± 0.03, a value that appears to be in excellent agreement both the Indebetouw et al. (2005) 2MASS reddening law, E(J − K)/E(H − K) = 1.78± 0.15, and with the Rieke & Lebofsky (1985) E(J − K)/E(H − K) = 1.70 normal reddening law converted into the 2MASS internal…”
A Spitzer Census of the IC 348 Nebula (2007, methodology): “Using a diskless K0 IC 348 member from Paper I (Table 3) as a template, we reddened the observed photosphere by extinctions as large as AV = 200 using the reddening law from Indebetouw et al. (2005).”
On Extending the Mass-Metallicity Relation of Galaxies by 2.5 Decades in Stellar Mass (2006, background): “We have also assumed zero extinction at 4.5 m (e.g., Lutz 1999; Indebetouw et al. 2005), and negligible contribution by diffuse H i Br emission to the overall galaxy flux (e.g., Lu et al. 2003; Lu 2004).”
Reddening and metallicity maps of the Milky Way bulge from VVV and 2MASS II. The complete high resolution extinction map and implications for Galactic bulge studies (2012, background): “Adopting 1.240, 1.664, and 2.164 micron as the effective wavelengths of a K2 giant (typical of red clump stars) for 2MASS from Indebetouw et al. (2005), the coefficients corresponding to the Cardelli et al. (1989) extinction law are AJ = 1.692E (J − Ks) , (1) AH = 1.054E (J − Ks) , (2) AKs = 0.689E…”
Pixie Dust: The Silicate Features in the Diffuse Interstellar Medium (2005, methodology): “Given the good agreement of the Indebetouw et al. (2005) and the Lutz (1999) extinction points, we combined them and carried out a least-squares fit assuming the same functional form as Indebetouw et al. (2005) and find log Ak/AKð Þ ¼ 0:65 2:40 log kþ 1:34 log kð Þ2.”
THE TENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA FROM THE SDSS-III APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT (2013, methodology): “…et al. 2003; Churchwell et al. 2009) and the Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010) λ = 4.5 μm data following the Rayleigh–Jeans Color Excess Method described in Majewski et al. (2011) and Zasowski et al. (2013) using the color extinction curve from Indebetouw et al. (2005).”
Spitzer Observations of IC 348: The Disk Population at 2-3 Million Years (2005, background): “The reddening law is a merger of empirical laws from Cardelli et al. (1989) for k < 1 m, RV ¼ 3:1 and from a Spitzer study by Indebetouw et al. (2005) for 1 m < k < 8 m.”
THE SPITZER SPACE TELESCOPE SURVEY OF THE ORION A AND B MOLECULAR CLOUDS. I. A CENSUS OF DUSTY YOUNG STELLAR OBJECTS AND A STUDY OF THEIR MID-INFRARED VARIABILITY (2012, background): “The value of AJ /AKs has been increased from the value of 2.5 reported in Indebetouw et al. (2005) to 2.65 for two reasons.”
VOSA: Virtual Observatory SED Analyzer. An application to the Collinder 69 open cluster (2008, methodology): “Visual extincion (AV in magnitudes) affecting the source: this value is used to deredden each SED (the Indebetouw et al. 2005 extinction law is applied).”
The initial conditions of stellar protocluster formation - I. A catalogue of Spitzer dark clouds (2009, methodology): “…in principle, the wavelength dependence of the dust extinction law, although recent work suggests thatfrom 4.5 to 8µm, the three last bands observed by Spitzer/IRAC, the extinction is a relatively flat function of wavelength (Lutzet al. 1996; Indebetouw et al. 2005; Román-Zúñiga et al. 2007).”
LIFTING THE DUSTY VEIL WITH NEAR- AND MID-INFRARED PHOTOMETRY. I. DESCRIPTION AND APPLICATIONS OF THE RAYLEIGH–JEANS COLOR EXCESS METHOD (2011, methodology): “The extinctions in each panel were actually measured via the color excess in (H−[4.5µ]), but translated from the selective to total extinction in the photometric band shown on the abscissa using the Indebetouw et al. (2005) extinction law.”
The COMPLETE Survey of Star-Forming Regions: Phase I Data (2006, methodology): “Note that for the NICER analysis we used a normal reddening law (Rieke & Lebofsky 1985); interestingly, this reddening law compares well with the newly determined 2MASS reddening law (Indebetouw et al. 2005, ; see also Lombardi et al. 2006).”
Spitzer Observations of NGC 1333: A Study of Structure and Evolution in a Nearby Embedded Cluster (2007, methodology): “This reddening law was adopted because it was consistently measured through several nearby, star-forming molecular clouds, and shown to be significantly different than the reddening law from diffuse ISM dust (Indebetouw et al. 2005).”
Galactic reddening in 3D from stellar photometry – an improved map (2018, methodology): “If, instead of assuming that AW2 = 0, we use the result from Indebetouw et al. (2005) that AH/AK = 1.55 to set the constant b, we arrive at AW2 = 0.12 mag for E(rP1 − zP1) = 1 mag.”
Infrared Extinction toward Nearby Star-forming Regions (2007, methodology): “In addition, we also give the extinction law for the l = 284 • off-cloud line of sight as derived by Indebetouw et al. (2005).”
A CATALOG OF EXTENDED GREEN OBJECTS IN THE GLIMPSE SURVEY: A NEW SAMPLE OF MASSIVE YOUNG STELLAR OBJECT OUTFLOW CANDIDATES (2008, methodology): “…via color selection in the GLIMPSE point source catalog and archive (e.g. Ellingsen 2006, 2007); and (2) due to the flat extinction curve between 4.5 and 8.0µm (Indebetouw et al. 2005), highly extincted stars could potentially appear green in 3.6/4.5/8.0µm color images (e.g. Rathborne et al. 2005).”
Interpreting Spectral Energy Distributions from Young Stellar Objects. II. Fitting Observed SEDs Using a Large Grid of Precomputed Models (2006, methodology): “We use an extinction model calculated with the method of Kim, Martin, & Hendry (1994) that fits a typical Galactic ISM curve modified for the mid-IR extinction properties derived by Indebetouw et al. (2005) (Wolff, private communication).”