Semi‐empirical analysis of Sloan Digital Sky Survey galaxies – I. Spectral synthesis method

By R. C. Fernandes, A. Mateus, L. Sodré, G. Stasińska, J. Gomes. 2005

948 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fa83dcb6822aa07dc4a1ad75208abd0296aa8601

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In Astronomy and Astrophysics

1. C. Conroy
2. M. Cappellari
3. P. Hopkins
4. L. Hernquist
5. P. V. van Dokkum
6. R. Dav'e
7. T. Naab
8. R. Somerville

In Instrumentation

1. C. Conroy
2. M. Cappellari
3. P. V. van Dokkum
4. P. Hopkins
5. L. Hernquist
6. R. Dav'e
7. T. Naab
8. M. Franx

Citations in the corpus

• Stellar Population Inference with Prospector (2020, methodology): “The optimization may be through non-linear or, for restricted models, linear methods, or a mix of both (Heavens et al. 2000; Cid Fernandes et al. 2005; Ocvirk et al. 2006; Tojeiro et al. 2007; Koleva et al. 2008).”
• Alternative diagnostic diagrams and the 'forgotten' population of weak line galaxies in the SDSS (2009, methodology): “We start from a raw sample of 926 246 galaxies analysed with the STARLIGHT code (Cid Fernandes et al. 2005) and apply an initial cut to objects within the SDSS Main Galaxy Sample (Strauss et al. 2002).”
• The ATLAS3D Project – XXX. Star formation histories and stellar population scaling relations of early-type galaxies (2015, methodology): “We overplot the linear relation given by de La Rosa et al. (2011), who conducted a similar analysis on SDSS spectra using the STARLIGHT code of Cid Fernandes et al. (2005).”
• The dependence of Type Ia Supernovae luminosities on their host galaxies (2010, background): “…potential well, ellipticals (or passively evolving galaxies) should follow the same general trend between stellar metallicity and Mstellar (Gallazzi et al. 2005), with stellar metallicity and gas-phase nebular metallicity well correlated (e.g. Cid Fernandes et al. 2005; Gallazzi et al. 2005).”
• THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I. HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS (2014, background): “As explained in Conroy (2013), while there has been extensive testing of spectra based SFH determinations (e.g, Cid Fernandes et al. 2005; Tojeiro et al. 2007), these tests have primarily focused on internal diagnostics (e.g., self-consistency between star-forming and quiescent galaxies,…”
• SUPERDENSE MASSIVE GALAXIES IN WINGS LOCAL CLUSTERS (2009, methodology): “REFERENCES Bell, E. F., & de Jong, R. S. 2001, ApJ, 550, 212 Bernardi, M. 2009, MNRAS, 395, 1491 Bezanson, R., van Dokkum, P. G., Tal, T., Marchesini, D., Kriek, M., Franx, M., & Coppi, P. 2009, ApJ, 697, 1290 Blanton, M. R., Schlegel, D. J., Strauss, M. A., Brinkmann, J., Finkbeiner, D., Fukugita, ”
• Systematic variation of the stellar initial mass function with velocity dispersion in early-type galaxies (2012, methodology): “In order to obtain an accurate estimate ofσ for each stack, we perform spectral fitting with the software STARLIGHT (Cid Fernandes et al. 2005), in the range 3800–8400Å.”
• UV-extended E-MILES stellar population models: young components in massive early-type galaxies (2016, background): “…stellar population parameters (e.g. Serven, Worthey & Briley 2005; Cervantes & Vazdekis 2009), including IMF indicators (e.g. La Barbera et al. 2013; Spiniello et al. 2014), and full spectrum-fitting (e.g. Cid Fernandes et al. 2005; Ocvirk et al. 2006a; Koleva et al. 2009; Tojeiro et al. 2011).”
• SUPERDENSE MASSIVE GALAXIES IN THE NEARBY UNIVERSE (2009, methodology): “To address this issue we have probed the Star Formation History (SFH) of our objects by means of STARLIGHT (Cid Fernandes et al. 2005) exploring which SSP-model combination best fits the observed spectra.”
• MIUSCAT: extended MILES spectral coverage – I. Stellar population synthesis models (2012, methodology): “In recent years it is becoming increasingly popular to use these model SEDs to derive relevant stellar population parameters, including the Star Formation History (SFH), by means of full spectrum-fitting approach (e.g., Cid Fernandes et al. 2005; Koleva et al. 2009; Tojeiro et al. 2011), which repre”
• Stellar population gradients in galaxy discs from the CALIFA survey - The influence of bars (2014, methodology): “In the past years, a series of papers have been published using 2D data from the VENGA (Blanc et al. 2010), the PINGS (Rosales-Ortega et al. 2010) and the CALIFA (Sánchez et al. 2012a,b) surveys where the star formation history of a sample of nearby galaxies of all morphological types has been studi”
• SPIDER VIII - constraints on the stellar initial mass function of early-type galaxies from a variety of spectral features (2013, methodology): “First, we measure the galaxy luminosity-weighted age by spectral fitting the wavelength range from 3900 to 7350 Å 10, with the STARLIGHT fitting code (Cid Fernandes et al. 2005).”
• The star formation history of CALIFA galaxies: Radial structures (2013, methodology): “The combined V1200 + V500 datacubes were processed as described in Cid Fernandes et al. (2013a).”
• How to Measure Galaxy Star Formation Histories. II. Nonparametric Models (2018, methodology): “The simplest nonparametric models fit directly for the mass formed in a series of piecewise constant functions (i.e., a step function) in time (Cid Fernandes et al. 2005; Ocvirk et al. 2006; Kelson et al. 2014; Leja et al. 2017; Chauke et al. 2018).”
• THE MASS–METALLICITY RELATION WITH THE DIRECT METHOD ON STACKED SPECTRA OF SDSS GALAXIES (2012, methodology): “We subtracted the stellar continuum with synthetic template galaxy spectra created with the starlight stellar synthesis code (Cid Fernandes et al. 2005), adopted the Cardelli et al. (1989) extinction law, and masked out the locations of the emission lines.”