K-Corrections and Filter Transformations in the Ultraviolet, Optical, and Near-Infrared

By M. Blanton, Sam T. Roweis. 2006

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Template fits to observed galaxy fluxes allow calculation of K-corrections and conversions among observations of galaxies at various wavelengths. We present a method for creating model-based template sets given a set of heterogeneous photometric and spectroscopic galaxy data. Our technique, nonnegative matrix factorization, is akin to principal component analysis (PCA), except that it is constrained to produce nonnegative templates, it can use a basis set of models (rather than the delta-function basis of PCA), and it naturally handles uncertainties, missing data, and heterogeneous data (including broadband fluxes at various redshifts). The particular implementation we present here is suitable for ultraviolet, optical, and near-infrared observations in the redshift range 0 < z < 1.5. Since we base our templates on stellar population synthesis models, the results are interpretable in terms of approximate stellar masses and star formation histories. We present templates fitted with this method to data from Galaxy Evolution Explorer, Sloan Digital Sky Survey spectroscopy and photometry, the Two Micron All Sky Survey, the Deep Extragalactic Evolutionary Probe, and the Great Observatories Origins Deep Survey. In addition, we present software for using such data to estimate K-corrections.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b16f1052aeb0c039263e0328d6b84d2292c1b15a

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Citations in the corpus

Stellar Mass—Halo Mass Relation and Star Formation Efficiency in High-Mass Halos (2014, methodology): “For galaxies with known redshifts the K-corrections were derived individually by using kcorrect (v 4.1.4) code (Blanton & Roweis 2007) and u, g, r, i, z-band fluxes derived from model magnitudes in SDSS catalog, while for the rest of galaxies we used the median mean K-correction of galaxies with…”
CALIFA : a diameter-selected sample for an integral field spectroscopy galaxy survey (2014, methodology): “We therefore calculated stellar masses using two existing and well-tested codes, namely kcorrect (Blanton & Roweis 2007) and an algorithm that has been extensively used and tested in Walcher et al. (2008, W08).”
Galaxy luminosities, stellar masses, sizes, velocity dispersions as a function of morphological type (2009, methodology): “A final estimate of M∗/Lr comes from Blanton & Roweis (2007), and is based on fitting the observed colours in all the SDSS bands to templates of a variety of star formation histories and metallicities, assuming the Chabrier (2003) IMF.”
How do galaxies populate dark matter haloes (2009, methodology): “17 of Blanton & Roweis (2007)).”
A New Sample of Low-Mass Black Holes in Active Galaxies (2007, methodology): “Once we have removed our best estimate for the AGN luminosity from the SDSS Petrosian magnitudes, we calculateKcorrections using the routines described in Blanton & Roweis (2007).”
Cosmological constraints from the 100-deg2 weak-lensing survey (2007, positive): “We employ the linear relationships between different filter bands given by Blanton & Roweis (2007): IAB = i ′ − 0.0647 − 0.7177[(i ′ − z′) − 0.2083], RVEGA = r ′ − 0.0576 − 0.3718[(r ′ − i ′) − 0.2589] − 0.21.”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, methodology): “Bond et al. (2010) analyzed the largest sample so far of halo star velocities within ∼10 kpc from the Sun, including ∼105 SDSS stars with three velocity components.”
Inferences on the timeline of reionization at z ∼ 8 from the KMOS Lens-Amplified Spectroscopic Survey (2019, positive): “…|m,µ, zd) = 1√ 2πσ2M exp [ − (Muv −Muv,mod(µ, zd)) 2 2σ2M ] (C5) where Muv,mod(µ, zd) = m−5 log10(DL/10 pc)+2.5 log10(1+ zd) + 2.5 log10 µ converts observed magnitudes to rest-frame UV magnitudes, assuming the UV spectral slope β = −2 to calculate the K-correction (e.g., Blanton & Roweis 2007).”
AEGIS-X: THE CHANDRA DEEP SURVEY OF THE EXTENDED GROTH STRIP (2008, methodology): “For sources not detected in the DEEP2 survey, but securely detected in the CFHTLS then we convert the CFHTLS r′AB magnitudes to RAB using R = r′ − 0.0576− 0.3718[(r′ − i′) − 0.2589] (6) (Blanton & Roweis 2007).”
J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817 (2017, methodology): “Using Lupton’s equation, the catalog magnitudes were converted from the PanSTARRS magnitude to the Johnson system.1 We converted Vega magnitudes to AB magnitudes using the method specified in Blanton and Roweis (2007).”
Cosmological parameter constraints from galaxy-galaxy lensing and galaxy clustering with the SDSS DR7 (2012, neutral): “• The k-corrections are to z = 0.1 (kcorrect v4 1 4; Blanton & Roweis 2007).”
Are Brightest Halo Galaxies Central Galaxies (2010, methodology): “All the magnitudes and colours of the galaxies are Petrosian, and they have been corrected for Galactic extinction (Schlegel, Finkbeiner & Davis 1998), and have been k-corrected and evolution-corrected to z = 0.1 (Blanton & Roweis 2007).”
UV Star Formation Rates in the Local Universe (2007, methodology): “In the current case, given that our redshift range is covered by only 5 model libraries, we choose to calculate the K corrections using the publicly available code KCORRECT V4_1_417 (Blanton & Roweis 2007).”
A strong redshift dependence of the broad absorption line quasar fraction (2010, methodology): “Non-negative matrix factorisation (NMF) is a relatively new BSS technique that incorporates a non-negativity constraint on both its components and their weights (Lee & Seung 1999, 2000; Blanton & Roweis 2007).”
Galaxy and Mass Assembly (GAMA): the GAMA galaxy group catalogue (G3Cv1) (2011, positive): “2 k-correction (Blanton & Roweis 2007) of GAMA-I galaxies, and ai(zref , zp) the coefficients of that polynomial fit.”
A CENSUS OF STAR-FORMING GALAXIES IN THE Z ∼ 9–10 UNIVERSE BASED ON HST+SPITZER OBSERVATIONS OVER 19 CLASH CLUSTERS: THREE CANDIDATE Z ∼ 9–10 GALAXIES AND IMPROVED CONSTRAINTS ON THE STAR FORMATION RATE DENSITY AT Z ∼ 9.2 (2012, methodology): “0 template set consists of five SED templates from PEGASE library (Fioc & Rocca-Volmerange 1997) derived based on the Blanton & Roweis (2007) algorithm and one young, dusty template (50 Myr, AV = 2.75).”
THE PRISM MULTI-OBJECT SURVEY (PRIMUS). I. SURVEY OVERVIEW AND CHARACTERISTICS (2010, methodology): “Restframe magnitudes are computed using the kcorrect software package (Blanton & Roweis 2007), which fits the sum of a set of basis templates at the PRIMUS redshift to the broadband optical photometry available in each field.”