Skip to main content
We gratefully acknowledge support from the Simons Foundation, member institutions, and all contributors. Donate

Astrophysics> Astrophysics of Galaxies

arXiv:1012.4804 (astro-ph)
[Submitted on 21 Dec 2010 (v1), last revised 22 Sep 2011 (this version, v2)]

Title:Measuring Reddening with SDSS Stellar Spectra and Recalibrating SFD

Authors:Edward F. Schlafly (1), Douglas P. Finkbeiner (1 and 2) ((1) Harvard Physics Department (2) Harvard-Smithsonian Center for Astrophysics)
View PDF
Abstract:We present measurements of dust reddening using the colors of stars with spectra in the Sloan Digital Sky Survey. We measure reddening as the difference between the measured and predicted colors of a star, as derived from stellar parameters from the SEGUE Stellar Parameter Pipeline (Lee et al. 2008a). We achieve uncertainties of 56, 34, 25, and 29 mmag in the colors u-g, g-r, r-i, and i-z, per star, though the uncertainty varies depending on the stellar type and the magnitude of the star. The spectrum-based reddening measurements confirm our earlier "blue tip" reddening measurements (Schlafly et al. 2010, S10), finding reddening coefficients different by -3%, 1%, 1%, and 2% in u-g, g-r, r-i, and i-z from those found by the blue tip method, after removing a 4% normalization difference. These results prefer an R_V=3.1 Fitzpatrick (1999) reddening law to O'Donnell (1994) or Cardelli et al. (1989) reddening laws. We provide a table of conversion coefficients from the Schlegel et al. (1998) maps of E(B-V) to extinction in 88 bandpasses for 4 values of R_V, using this reddening law and the 14% recalibration of SFD first reported by S10 and confirmed in this work.
Comments: 14 pages, 8 figures (arxiv version updated to published version)
Subjects: Astrophysics of Galaxies (astro-ph.GA)
Cite as: arXiv:1012.4804 [astro-ph.GA]
(or arXiv:1012.4804v2 [astro-ph.GA] for this version)
https://doi.org/10.48550/arXiv.1012.4804
Related DOI: https://doi.org/10.1088/0004-637X/737/2/103

Submission history

From: Edward Schlafly [view email]
[v1] 2010年12月21日 21:00:01 UTC (698 KB)
[v2] 2011年9月22日 21:24:18 UTC (592 KB)
Full-text links:

Access Paper:

  • View PDF
  • TeX Source
  • Other Formats
Current browse context:
astro-ph.GA
Change to browse by:

References & Citations

export BibTeX citation

Bibliographic and Citation Tools

Bibliographic Explorer (What is the Explorer?)
Connected Papers (What is Connected Papers?)
Litmaps (What is Litmaps?)
scite Smart Citations (What are Smart Citations?)

Code, Data and Media Associated with this Article

alphaXiv (What is alphaXiv?)
CatalyzeX Code Finder for Papers (What is CatalyzeX?)
DagsHub (What is DagsHub?)
Gotit.pub (What is GotitPub?)
Hugging Face (What is Huggingface?)
Papers with Code (What is Papers with Code?)
ScienceCast (What is ScienceCast?)

Demos

Replicate (What is Replicate?)
Hugging Face Spaces (What is Spaces?)
TXYZ.AI (What is TXYZ.AI?)

Recommenders and Search Tools

Influence Flower (What are Influence Flowers?)
CORE Recommender (What is CORE?)
IArxiv Recommender (What is IArxiv?)

arXivLabs: experimental projects with community collaborators

arXivLabs is a framework that allows collaborators to develop and share new arXiv features directly on our website.

Both individuals and organizations that work with arXivLabs have embraced and accepted our values of openness, community, excellence, and user data privacy. arXiv is committed to these values and only works with partners that adhere to them.

Have an idea for a project that will add value for arXiv's community? Learn more about arXivLabs.

AltStyle によって変換されたページ (->オリジナル) /