The stellar masses of 25 000 galaxies at 0.2 ≤ z ≤ 1.0 estimated by the COMBO-17 survey

By A. Borch, K. Meisenheimer, Eric F. Bell, Hans-Walter Rix, Christian Wolf, S. Dye, M. Kleinheinrich, Z. Kovács, L. Wisotzki. 2006

240 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f6dbcc69af0f3145acaf59433663aac5a33e08ef

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Somerville
4. C. Conroy
5. R. Dav'e
6. P. V. van Dokkum
7. A. Dekel
8. Thomas J. Cox

In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. C. Conroy
4. R. Somerville
5. P. V. van Dokkum
6. R. Dav'e
7. Thomas J. Cox
8. A. Dekel

Citations in the corpus

• The many manifestations of downsizing: hierarchical galaxy formation models confront observations (2009, methodology): “In more recent times, most mass estimates (Drory et al. 2004, 2005; Borch et al. 2006; Bundy et al. 2006; Fontana et al. 2006; Marchesini et al. 2008; Pérez-González et al. 2008) have been based on multiwavelength spectral energy distribution (SED) fitting algorithms.”
• THE RISE AND FALL OF PASSIVE DISK GALAXIES: MORPHOLOGICAL EVOLUTION ALONG THE RED SEQUENCE REVEALED BY COSMOS (2009, background): “…since z ∼ 2 of the two populations as partitioned by the amount of star formation or the rest-frame color (Juneau et al. 2005; Bundy et al. 2006; Borch et al. 2006; Willmer et al. 2006; Brown et al. 2007; Ilbert et al. 2010; Mobasher et al. 2009) and as a function of morphological type (Bundy…”
• MERGERS AND BULGE FORMATION IN ΛCDM: WHICH MERGERS MATTER? (2009, background): “The specific choices are not important – we could just as well use a number of other observations in the literature (e.g. Bundy et al. 2005; Pannella et al. 2006; Franceschini et al. 2006; Borch et al. 2006; Fontana et al. 2006; Brown et al. 2007; Marchesini et al. 2009; Kajisawa et al. 2009).”
• The importance of satellite quenching for the build-up of the red sequence of present-day galaxies (2007, background): “…et al. 2004; Tanaka et al. 2005; Cooper et al. 2006; Cucciati et al. 2006; Willmer et al. 2006), and that the total stellar mass density on the red sequence has roughly doubled over the last 6–8 Gyr (e.g. Bell et al. 2004; Borch et al. 2006; Zucca et al. 2006; Brown et al. 2007; Faber et al. 2007).”
• THE GREATER IMPACT OF MERGERS ON THE GROWTH OF MASSIVE GALAXIES: IMPLICATIONS FOR MASS ASSEMBLY AND EVOLUTION SINCE z ≃ 1 (2009, background): “…early completion of star formation in the most massive galaxies, followed by continued activity in lower-mass systems—a phenomenon now termed “downsizing” (e.g., Juneau et al. 2005; Treu et al. 2005; Bundy et al. 2006; Borch et al. 2006; Cimatti et al. 2006; Bell et al. 2007; Cowie & Barger 2008).”
• DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS OF SPHEROIDS (2008, background): “…(2006) and Vale & Ostriker (2006) at different redshifts from each of the the observed mass functions of Fontana et al. (2006); Bundy et al. (2005); Borch et al. (2006); Blanton (2006) (see Hopkins et al. 2008f), and have also found similar results assuming no evolution inP(Mgal|Msubhalo) (for…”
• Star Formation and the Growth of Stellar Mass (2007, methodology): “…for a critical discussion of this issue), the evolution of total stellar mass in the universe is reasonably well reproduced by the integrated cosmic-averaged star formation rate (SFR), provided that one accounts for stellar mass loss (Cole et al. 2001; Rudnick et al. 2003; Borch et al. 2006).”
• The Evolving Luminosity Function of Red Galaxies (2006, result): “However, unlike some recent studies (e.g., Bundy et al. 2006; Borch et al. 2006; Cimatti et al. 2006), we do see evidence for the ongoing assembly of the most massive red galaxies, albeit at a rate that produces little growth of 4L red galaxy stellar masses at z < 1.”
• The Stellar Mass Assembly of Galaxies from z = 0 to z = 4: Analysis of a Sample Selected in the Rest-Frame Near-Infrared with Spitzer (2007, methodology): “Indeed, Borch et al. (2006) find good agreement between the SFR and the stellar mass density evolution at z<1 by choosing a Chabrier (2003) IMF, which gives stellar masses similar to a Kroupa et al. (1993) IMF (∼1.7 times lower than our masses, based on a Salpeter IMF), but with lower SFRs (by a…”
• The UV-Optical Color Magnitude Diagram. II. Physical Properties and Morphological Evolution On and Off of a Star-forming Sequence (2007, unknown): “In the limit SFR/M⋆ → 0, Φ(> SFR/M⋆, M⋆) → φ(M⋆) which shows good agreement with the local stellar mass function derived by Borch et al. (2006) (taken from Bell et al. 2003b).”
• The galaxy stellar mass-star formation rate relation: evidence for an evolving stellar initial mass function? (2007, background): “Borch et al. (2006) also noted such tension, but suggested that switching from Salpeter to a Chabrier or Kroupa IMF might go significantly towards reconciling the difference, little evidence exists for IMF evolution to z 1 (Bell et al. 2007).”
• THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 ⩽ z ⩽ 2.2 (2011, background): “It is clear that red (quiescent) and blue (star-forming) samples selected using theUVJ colors will be different from those based on a single rest-frame color, as was done by, e.g., Bell et al. (2004) and Borch et al. (2006).”
• Compact high-redshift galaxies are the cores of the most massive present-day spheroids (2009, background): “…nor is there significant evolution in the (uniformly old) stellar populations, or any significant stellar mass loss or new star formation given the old stellar population ages (Nelan et al. 2005; Thomas et al. 2005; Gallazzi et al. 2006; Masjedi et al. 2006; Borch et al. 2006; Jones et al. 2006).”
• COLOR–MAGNITUDE RELATIONS OF ACTIVE AND NON-ACTIVE GALAXIES IN THE CHANDRA DEEP FIELDS: HIGH-REDSHIFT CONSTRAINTS AND STELLAR-MASS SELECTION EFFECTS (2010, methodology): “…scatter, which is adequate for our purposes in this work.19 We speculate that the offset of mass scale may arise from the subtle differences in the IMF and the random scatter may mostly be due to the fact that we are using different photometric redshifts from those used by Borch et al. (2006).”
• Systematic investigation of the expected gravitational wave signal from supermassive black hole binaries in the pulsar timing band (2012, methodology): “We take three different galaxy stellar mass functions from the literature (Borch et al. 2006; Drory et al. 2009; Ilbert et al. 2010) and match them with the local mass function (Bell et al. 2003), to obtain three fiducialφz(M).”
• Galaxy Groups in the SDSS DR4. I. The Catalog and Basic Properties (2007, methodology): “…− 4.64) , (2) Here 0.0(g − r) and 0.0Mr − 5 logh are the (g − r) color and r-band magnitude K + E corrected to z = 0.0, 4.64 is the r-band magnitude of the Sun in the AB system (Blanton & Roweis 2007), and the −0.10 term effectively implies that we adopt a Kroupa (2001) IMF (Borch et al. 2006).”
• THE STRUCTURE OF THE MILKY WAY'S HOT GAS HALO (2013, background): “This opposes the observed cosmic SFR, indicating that the halo is likely not entirely at a solar metallicity (Borch et al. 2006).”