Photometric Separation of Stellar Properties Using SDSS Filters

Lenz, Dawn D.; Newberg, Jo; Rosner, R.; Richards, Gordon T.; Stoughton, Chris

doi:10.1086/313155

Cited by 106 publications

(156 citation statements)

References 12 publications

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“…The large scatter in the U − B residual is partly due to variable stars and partly due to the low signal-to-noise region in the U band. The Lenz et al (1998) …”

Section: Photometric Comparisonmentioning

confidence: 99%

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The X-shooter Spectral Library (XSL)

Chen

Trager

Peletier

et al. 2014

A&A

109

117

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We present the first release of the X-shooter Spectral Library (XSL). This release contains 237 stars. The spectra in this release span a wavelength range of 3000-10 200 Å and have been observed at a resolving power of R ≡ λ/Δλ ∼ 10 000. The spectra were obtained at ESO's 8-m Very Large Telescope (VLT). The sample contains O-M, long-period variable, C and S stars. The spectra are flux-calibrated and telluric-corrected. We describe a new technique for the telluric correction. The wavelength coverage, spectral resolution, and spectral type of this library make it well suited to stellar population synthesis of galaxies and clusters, kinematical investigation of stellar systems, and the study of the physics of cool stars.

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“…The large scatter in the U − B residual is partly due to variable stars and partly due to the low signal-to-noise region in the U band. The Lenz et al (1998) …”

Section: Photometric Comparisonmentioning

confidence: 99%

“…Since there are few literature stars, which have the SDSS colors in common with our sample, we use the model colors computed by Lenz et al (1998) as a rough check. Models with log g = 4.5 and log g = 2.5 are chosen to represent the main sequence and giants, respectively.…”

Section: Photometric Comparisonmentioning

confidence: 99%

The X-shooter Spectral Library (XSL)

Chen

Trager

Peletier

et al. 2014

A&A

109

117

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“…First, the star with very blue colors (lower left on each plot) has an SDSS spectrum of a high-temperature blackbody (T eff ≳ 40; 000 K) with slight Balmer absorption features and has to be either a very hot O star or white dwarf. Its colors based on SDSS filters place it at the extreme end of the main sequence based on both comparison with known stars and with stellar models (Lenz et al 1998;Covey et al 2007), and it is in the Bianchi et al (2011) catalog of potential hot white dwarfs. In the latter catalog, its FUV-NUV and NUV colors indicate T eff ≳ 40; 000 K, which matches the SDSS spectrum and full photometry from GALEX, XMM-OM, and the SDSS.…”

Section: Color-color Diagrams and Noncluster Object Characterizationmentioning

confidence: 99%

Using theXMM-NewtonOptical Monitor to Study Cluster Galaxy Evolution

Miller

O’Steen²,

Yen

et al. 2012

Publications of the Astronomical Society of the Pacific

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ABSTRACT. We explore the application of XMM-Newton Optical Monitor (XMM-OM) ultraviolet (UV) data to study galaxy evolution. Our sample is constructed as the intersection of all Abell clusters with z < 0:05 and having archival XMM-OM data in either the UVM2 or UVW1 filters, plus optical and UV photometry from the Sloan Digital Sky Survey and GALEX, respectively. The 11 resulting clusters include 726 galaxies with measured redshifts, 520 of which have redshifts placing them within their parent Abell clusters. We develop procedures for manipulating the XMM-OM images and measuring galaxy photometry from them, and we confirm our results via comparison with published catalogs. Color-magnitude diagrams (CMDs) constructed using the XMM-OM data along with SDSS optical data show promise for evolutionary studies, with good separation between red and blue sequences and real variation in the width of the red sequence that is likely indicative of differences in star formation history. This is particularly true for UVW1 data, as the relative abundance of data collected using this filter and its depth make it an attractive choice. Available tools that use stellar synthesis libraries to fit the UV and optical photometric data may also be used, thereby better describing star formation history within the past billion years and providing estimates of total stellar mass that include contributions from young stars. Finally, color-color diagrams that include XMM-OM UV data appear useful to the photometric identification of both extragalactic and stellar sources.

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“…The z ′ band is well-suited for discovery of objects beyond the current distance record of z∼5, as continuum absorption shortward of Lyα then suppresses images in other of the filters, and the very strong observed Lyα emission typical of high-z QSOs is concentrated in just one band. Considerable early work, both theoretical (Newberg & Yanny 1997, Lenz et al 1998) and observational (Richards et al 1997, Newberg et al 1997, Krisciunas et al 1998) has already been invested in delineating the normal stellar locus, as well as the positions of a variety of interesting objects, in this photometric system, as this information is essential for efficient, autonomous selection of large numbers of unresolved images for many of the Survey's spectroscopic programs, as well as for transformation of SDSS magnitudes to other systems.…”

Section: (A ) Scientific Goalsmentioning

confidence: 99%

The Sloan Digital Sky Survey

Szalay

2001

Structure Formation in the Universe

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Photometric Separation of Stellar Properties Using SDSS Filters

Cited by 106 publications

References 12 publications

The X-shooter Spectral Library (XSL)

The X-shooter Spectral Library (XSL)

Using theXMM-NewtonOptical Monitor to Study Cluster Galaxy Evolution

The Sloan Digital Sky Survey

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