The Sloan Digital Sky Survey monitor telescope pipeline

Tucker, D. L.; Kent, Stephen M.; Richmond, M.; Annis, J.; Smith, J. Allyn; Allam, S.; Rodgers, Christopher T.; Stute, J. L.; Adelman-McCarthy, Jennifer K.; Brinkmann, J.; Doi, Mamoru; Finkbeiner, Douglas P.; Fukugita, M.; Goldston, J. E.; Greenway, B.; Gunn, James E.; Hendry, John S.; Hogg, David W.; Ichikawa, S.; Ivezić, Željko; Knapp, G. R.; Lampeitl, H.; Lee, B.C.; Lin, Huan; McKay, Timothy A.; Merrelli, Aronne; Munn, Jeffrey A.; Neilsen, Eric H.; Newberg, Heidi Jo; Richards, Gordon T.; Schlegel, David J.; Stoughton, Chris; Uomoto, Alan; Yanny, B.

doi:10.1002/asna.200610655

Cited by 336 publications

(281 citation statements)

References 39 publications

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“…A custom photometric pipeline (Photo; Lupton et al 2001) was constructed to analyze each image and perform photometry. Calibration onto a standard star network (Smith et al 2002) was accomplished using observations from the "Photometric Telescope" (PT; Hogg et al 2001;Tucker et al 2006). Further discussion of PT calibrations for low-mass stars can be found in Davenport et al (2007).…”

Section: Sdss Photometrymentioning

confidence: 99%

“…Instead, the 0.5m Photometric Telescope (PT) was used to obtain (ugriz) ′ photometry 11 of these stars. The PT was active every night the 2.5m telescope was used in imaging mode during the SDSS, observing patches of the nightly footprint to determine the photometric solution for the night and to calibrate the zero-point of the 2.5m observations (Smith et al 2002;Tucker et al 2006). Golimowski et al (2010) obtained (ugriz) ′ photometry of the parallax sample over 20 nights for 268 low-mass stars.…”

Section: Photometric Telescope Photometrymentioning

confidence: 99%

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The Luminosity and Mass Functions of Low-Mass Stars in the Galactic Disk. Ii. The Field

Bochanski¹,

Hawley²,

Covey³

et al. 2010

The Astronomical Journal

322

305

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We report on new measurements of the luminosity function (LF) and mass function (MF) of field low-mass dwarfs derived from Sloan Digital Sky Survey (SDSS) Data Release 6 (DR6) photometry. The analysis incorporates ∼ 15 million low-mass stars (0.1 M ⊙ < M < 0.8M ⊙ ), spread over 8,400 square degrees. Stellar distances are estimated using new photometric parallax relations, constructed from ugriz photometry of nearby low-mass stars with trigonometric parallaxes. We use a technique that simultaneously measures Galactic structure and the stellar LF from 7 < M r < 16. We compare the LF to previous studies and convert to a MF using the mass-luminosity relations of Delfosse et al. (2000). The system MF, measured over −1.0 < log M/M ⊙ < −0.1, is well-described by a log-normal distribution with M • = 0.25 M ⊙ . We stress that our results should not be extrapolated to other mass regimes. Our work generally agrees with prior low-mass stellar MFs and places strong constraints in future star-formation studies of the Milky Way.

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Section: Sdss Photometrymentioning

confidence: 99%

Section: Photometric Telescope Photometrymentioning

confidence: 99%

The Luminosity and Mass Functions of Low-Mass Stars in the Galactic Disk. Ii. The Field

Bochanski¹,

Hawley²,

Covey³

et al. 2010

The Astronomical Journal

322

305

View full text Add to dashboard Cite

show abstract

“…The latter defines the unprimed ugriz system for which photometry has been published from SDSS DR1 onward, and for which we provide synthetic colours in this work. Primed magnitudes should thus be transformed into the unprimed system before comparing and/or using them with the synthetic photometry published here (see e.g., Tucker et al 2006). …”

Section: Sloan Digital Sky Survey Ugrizmentioning

confidence: 99%

Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

Casagrande¹,

VandenBerg²

2014

Monthly Notices of the Royal Astronomical Society

257

321

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After a pedagogical introduction to the main concepts of synthetic photometry, colours and bolometric corrections in the Johnson-Cousins, 2MASS, and HST-ACS/WFC3 photometric systems are generated from MARCS synthetic fluxes for various [Fe/H] and [α/Fe] combinations, and virtually any value of E(B − V) 0.7. The successes and failures of model fluxes in reproducing the observed magnitudes are highlighted. Overall, extant synthetic fluxes predict quite realistic broad-band colours and bolometric corrections, especially at optical and longer wavelengths: further improvements of the predictions for the blue and ultraviolet spectral regions await the use of hydrodynamic models where the microturbulent velocity is not treated as a free parameter. We show how the morphology of the colour-magnitude diagram (CMD) changes for different values of [Fe/H] and [α/Fe]; in particular,how suitable colour combinations can easily discriminate between red giant branch and lower main sequence populations with different [α/Fe], due to the concomitant loops and swings in the CMD. We also provide computer programs to produce tables of synthetic bolometric corrections as well as routines to interpolate in them. These colour-T eff -metallicity relations may be used to convert isochrones for different chemical compositions to various bandpasses assuming observed reddening values, thus bypassing the standard assumption of a constant colour excess for stars of different spectral type. We also show how such an assumption can lead to significant systematic errors. The MARCS transformations presented in this study promise to provide important constraints on our understanding of the multiple stellar populations found in globular clusters (e.g., the colours of lower main sequence stars are predicted to depend strongly on [α/Fe]) and of those located towards/in the Galactic bulge.

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“…A large WD sample of known completeness is required to determine a precise LF to address these questions. Luckily, the Sloan Digital Sky Survey (SDSS) (Gunn et al 1998(Gunn et al , 2006York et al 2000;Stoughton et al 2002;Pier 2003;Tucker et al 2006) provides the perfect sample for this effort. Although primarily designed as an extra-Galactic survey, the SDSS is an extremely rich source of stellar (and in particular, white dwarf) spectra.…”

Section: Introductionmentioning

confidence: 99%

A hot white dwarf luminosity function from the Sloan Digital Sky Survey

Krzesiński¹,

Kleinman²,

Nitta³

et al. 2009

A&A

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Aims. We present a hot white dwarf (WD) luminosity function (LF) using data taken from the Sloan Digital Sky Survey (SDSS) Data Release 4. We present and discuss a combined LF, along with separate DA and non-DA as LFs. We explore the completeness of our LFs and interpret a sudden drop in the non-DA LF near 2 M bol as a transition of the non-DA WD atmosphere into the DA one during WD evolution. Our LF extends roughly between −0.5 < M bol < 7 or equivalently, ∼120 000 K > T eff > ∼25 000 K. Our LF should now be useful for estimates of recent star formation and for studies of neutrino and other potential particle emission losses in hot WDs. Methods. To create a sample whose completeness can be characterized fully, we used stars whose spectra were obtained via the SDSS's "hot standard" target selection criteria. The hot standard stars were purposefully targeted to a high level of completeness by the SDSS for calibration purposes. We are fortunate that many of them are hot white dwarfs stars. We further limited the sample to stars with fitted temperatures exceeding 23 500 K and log g > 7.0. We determined stellar distances for our sample based on their absolute SDSS g filter magnitudes, derived from WD stellar atmosphere model fits to the SDSS stellar spectra. Results. We compared our LF with those of other researchers where overlap occurs; however, our LFs are unique in their extension to the most luminous/hottest WDs. The cool end of our LF connects with the hot end of previously determined SDSS WD LFs and agreement here is quite good. It is also good with previous non-SDSS WD LFs. We note distinct differences between the DA and non-DA LFs and discuss the reliability of the DA LF at its hot end. We have extended the range of luminosities covered in the most recent WD LFs. The SDSS sample is understood quite well and its exploration should contribute to a number of new insights into early white dwarf evolution.

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The Sloan Digital Sky Survey monitor telescope pipeline

Cited by 336 publications

References 39 publications

The Luminosity and Mass Functions of Low-Mass Stars in the Galactic Disk. Ii. The Field

The Luminosity and Mass Functions of Low-Mass Stars in the Galactic Disk. Ii. The Field

Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

A hot white dwarf luminosity function from the Sloan Digital Sky Survey

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