Hubble Space Telescope Absolute Spectrophotometry of Vega from the Far-Ultraviolet to the Infrared

By R. Bohlin, R. Gilliland. 2004

182 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/c69fc36b15385545dc02cc06f2bd543af8078b4f

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In Astronomy and Astrophysics

1. A. Riess
2. C. Conroy
3. A. Filippenko
4. R. Kirshner
5. S. Jha
6. P. V. van Dokkum
7. M. Cappellari
8. T. Treu

In Atmospheric Science

1. Pierre Bergeron
2. Luca Casagrande
3. Chris Flynn
4. M. Bessell
5. J. Holberg
6. Stephen J. Warren
7. Paul Hewett
8. P.-E. Tremblay

Citations in the corpus

• Accurate fundamental parameters for lower main‐sequence stars (2006, methodology): “This model has recently shown excellent agreement with the STIS flux distribution over the range 0.17–1.01 µm (Bohlin & Gilliland 2004).”
• M dwarfs: effective temperatures, radii and metallicities (2008, methodology): “In this work we have updated the absolute calibration of Vega in the optical by adopting the new reference spectra of Bohlin (2007) rather than that of Bohlin & Gilliland (2004) and which is expected to be accurate within ∼ 1 percent in the range 3200 − 10000 Å.”
• The Supernova Legacy Survey: Measurement of Omega_M, Omega_Lambda,and w from the First Year Data Set (2005, background): “Some subtle differences are found by a more recent HST measurement (Bohlin & Gilliland 2004) but they only marginally affect broadband photometry: differences within the 1% uncertainty quoted in Hayes (1985) are found and we will assign this uncertainty to the Vega broadband fluxes.”
• THE CARNEGIE SUPERNOVA PROJECT: SECOND PHOTOMETRY DATA RELEASE OF LOW-REDSHIFT TYPE Ia SUPERNOVAE (2010, methodology): “In doing so, we use the Bohlin & Gilliland (2004) SED of Vega (version 5) obtained from CALSPEC17, and the Fukugita et al. (1996) standard magnitudes Bstd = 0.03 and Vstd= 0.03.”
• Effective temperature scale and bolometric corrections from 2MASS photometry (2006, methodology): “Bohlin & Gilliland (2004) pointed out a probable 2% overestimation of the IR flux in the Vega model used by Cohen et al. (2003a).”
• Gaia broad band photometry (2010, background): “In that way,G =GBP=GRP=GRVS= V = 0.03 mag for a Vega-like 3 Bohlin & Gilliland (2004) give a value ofV = 0.026± 0.008 for the same flux at 555.6 nm, and Bohlin (2007) gives a revised value V = 0.023± 0.008 mag. star.”
• The Carnegie Supernova Project: Absolute Calibration and the Hubble Constant (2018, methodology): “Typically the Bohlin & Gilliland (2004b) SED of Vega is used for the set B, V , Y , J , H, while the Bohlin & Gilliland (2004a) SED of BD + 17◦4708 is used for u, g , r, and i.”
• Calibration of Synthetic Photometry Using DA White Dwarfs (2005, methodology): “…of these stars are in turn linked to the absolute flux of Vega through normalization to Landolt’s carefully measured V magnitudes (see Bohlin 2000; Bohlin & Gilliland 2004, hereafter BG04) and constitute a self-consistent, absolutely calibrated scale encompassing wavelengths from the optical to…”
• HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, methodology): “NGSL spectra cover 2000–10000 Åwith spectrophotometric precision of 0.5% (Bohlin et al. 2001; Bohlin & Gilliland 2004a, 2004b).”
• Observational Constraints on the Nature of Dark Energy: First Cosmological Results from the ESSENCE Supernova Survey (2007, methodology): “We here use MLCS2k2 v004 with the Bohlin & Gilliland (2004) values for the mag- nitudes of Vega: i.e., alpha_lyr_stis_002.fits with RVega = 0.033 mag.”
• A SPECTROSCOPIC SURVEY AND ANALYSIS OF BRIGHT, HYDROGEN-RICH WHITE DWARFS (2011, methodology): “Synthetic colors are obtained using the procedure outlined in Holberg & Bergeron (2006) based on the Vega fluxes taken from Bohlin & Gilliland (2004).”
• New Hubble Space Telescope Discoveries of Type Ia Supernovae at z ≥ 1: Narrowing Constraints on the Early Behavior of Dark Energy (2006, methodology): “Second, we adopted an updated zero point for the HST ACS Vegamag photometric system from Sirianni et al. (2005), which uses the spectrophotometry of Vega from Bohlin & Gilliland (2004) and improved quantum efficiency data for ACS to set Vega to 0.00 mag in all passbands.”
• KNOW YOUR NEIGHBORHOOD: A DETAILED MODEL ATMOSPHERE ANALYSIS OF NEARBY WHITE DWARFS (2012, methodology): “Synthetic colors are then obtained using the procedure outlined in Holberg & Bergeron (2006) based on the Vega fluxes taken from Bohlin & Gilliland (2004).”
• Bright OB stars in the Galaxy. III. Constraints on the radial stratification of the clumping factor (2006, methodology): “The available V-band magnitudes of Vega range from 0 .m026 (Bohlin & Gilliland 2004) to 0 .m035 (Colina & Bohlin 1994), while in the present investigation we adopt V = 0 .m03 mag in agreement with Johnson et al. (1966b).”
• THE CARNEGIE SUPERNOVA PROJECT: FIRST PHOTOMETRY DATA RELEASE OF LOW-REDSHIFT TYPE Ia SUPERNOVAE (2009, methodology): “We are therefore on a Vega system and use the Bohlin & Gilliland (2004a) SED.”
• Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters (2006, methodology): “In order to constrain the non-trivial problem of using an accurate zero point for the B and V filters, we used the SED from Bohlin & Gilliland (2004), based on high-S/N STIS observations and extrapolated to higher wavelengths, using Kurucz model atmospheres.”
• The UKIRT wide field camera ZYJHK photometric system: calibration from 2MASS (2008, methodology): “The spectrum for Vega is the same used by Hewett et al. (2006), originally from Bohlin & Gilliland (2004).”