Near-infrared template spectra of normal galaxies: k-corrections, galaxy models and stellar populations

By F. Mannucci, F. Basile, B. Poggianti, A. Cimatti, E. Daddi, L. Pozzetti, L. V. CAISMI-CNR, Firenze, U. Firenze, O. Padova and 4 more. 2001

231 citations recorded by the source corpus.

We have observed 28 local galaxies in the wavelength range between 1 and 2.4 μm in order to define template spectra of the normal galaxies along the Hubble sequence. Five galaxies per morphological type were observed in most cases, and the resulting rms spread of the normalized spectra of each class, including both intrinsic differences and observational uncertainties, is about 1 per cent in K, 2 per cent in H and 3 per cent in J. Many absorption features can be accurately measured. The target galaxies and the spectroscopic aperture (7×53 arcsec2) were chosen to be similar to those used by Kinney et al. to define template UV and optical spectra. The two data sets are matched in order to build representative spectra between 0.1 and 2.4 μm. The continuum shape of the optical spectra and the relative normalization of the near-IR ones were set to fit the average effective colours of the galaxies of the various Hubble classes. The resulting spectra are used to compute the k-corrections of the normal galaxies in the near-IR bands, and to check the predictions of various spectral synthesis models: while the shape of the continuum is generally well predicted, large discrepancies are found in the absorption lines. Among the other possible applications, here we also show how these spectra can be used to place constraints on the dominant stellar population in local galaxies. Spectra and k-corrections are publicly available and can be downloaded from the web site http://www.arcetri.astro.it/~filippo/spectra.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/62221c51e713791b48b5656cbcc73d4c8ba5c862

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Renzini
2. P. Hopkins
3. L. Hernquist
4. C. Conroy
5. E. Daddi
6. Simon D. M. White
7. Volker Springel
8. R. Dav'e

In Instrumentation

1. A. Renzini
2. C. Conroy
3. E. Daddi
4. P. Hopkins
5. L. Hernquist
6. A. Cimatti
7. Simon D. M. White
8. R. Dav'e

Citations in the corpus

• Are the hosts of gamma-ray bursts sub-luminous and blue galaxies? (2003, methodology): “To compute the evolution of their R−K colours with redshift, we used the optical/NIR templates of Mannucci et al. (2001) for the E and Sc types, and the optical Scd and Irr SEDs of Coleman et al. (1980).”
• The UKIRT Infrared Deep Sky Survey ZY JHK photometric system: passbands and synthetic colours (2006, background): “The second set of templates are the spectra created by Mannucci et al. (2001), by combining their near-infrared aver- aged spectra with the UV–optical template spectra of Kinney et al. (1996).”
• A Combined Optical and X-ray Study of Unobscured Type 1 AGN. I. Optical Spectra and SED Modeling (2011, background): “…Bian & Huang 2010), but these studies also needed to include additional contributions from the host galaxy and emission from the dusty torus to account for the extra continuum emission at long wavelengths of the optical spectrum (e.g. Kinney et al. 1996; Mannucci et al. 2001; Landt et al. 2011).”
• THE ACS NEARBY GALAXY SURVEY TREASURY (2007, methodology): “K-band total magnitudes were adopted from Jarrett et al. (2003) or Vaduvescu et al. (2005) when available, or inferred from B band magnitudes assuming B −K ∼ 2.86, based on the estimates in Mannucci et al. (2001) for dwarf irregular spectral types.”
• Age and Metallicity Distribution of the Galactic Bulge from Extensive Optical and Near-IR Stellar Photometry (2002, result): “Figure 22 shows the resulting spectral energy distribution (SED) of the galactic bulge, compared to the template spectra of elliptical, Sa and Sc galaxies from Mannucci et al. (2001).”
• The quasar relation through cosmic time – II. Evidence for evolution from z = 3 to the present age (2009, methodology): “…quasar in the cosmological frame we adopted, C(z) is a term accounting for filter and kcorrection, as derived by assuming an elliptical galaxy template (Mannucci et al. 2001), and Af is a term accounting for the Galactic extinction, as derived from the H i maps in Schlegel Finkbeiner & Davis…”
• A simplified view of blazars: clearing the fog around long‐standing selection effects (2011, methodology): “For the spectral shape we used the galaxy tem- c© 2011 RAS, MNRAS 000, 1–14 plate of Mannucci et al. (2001), who derived it combining the data from 28 local elliptical galaxies observed in the wavelength range 0.12 − 2.4 µm.”
• Simultaneous Planck, Swift, and Fermi observations of X-ray and γ-ray selected blazars (2011, methodology): “For the spectral shape, we used the elliptical galaxy template of Mannucci et al. 2001 (bottom panel of Fig.”
• The K20 survey. V. The evolution of the near-IR Luminosity Function (2003, methodology): “The small variance ofk-corrections in theKs-band (Cowie et al. 1994; Mannucci et al. 2001) greatly simplifies the analysis with respect to optically-selected samples of galaxies.”
• The evolution of the luminosity functions in the FORS Deep Field from low to high redshift: I. The blue bands (2004, methodology): “As templates we used (a) local galaxy templates from Mannucci et al. (2001), and Kinney et al. (1996) and (b) semi-empirical templates more appropriate for modest to high redshift galaxies.”
• A Near-Infrared Spectral Template for Quasars (2005, methodology): “We useM Ks ¼ 23:47 for early-type galaxies (Kochanek et al. 2001) and scale the elliptical galaxy template spectrum from Mannucci et al. (2001), which spans ultraviolet to near-infrared wavelengths, by its K-band flux to the flux expected from an 2L galaxy at the redshift of each quasar.”
• TRACING OUTFLOWS AND ACCRETION: A BIMODAL AZIMUTHAL DEPENDENCE OF Mg ii ABSORPTION (2012, unknown): “When only one color was measured, we applied a conversion determined from a linear least-squares fit to the average colors from galaxy spectral energy distribution templates of Mannucci et al. (2001).”
• The FIRST-2MASS Red Quasar Survey (2007, methodology): “We conducted a two-component fit to our spectra, using the same quasar template plus an elliptical galaxy template from Mannucci et al. (2001), allowing the reddening and fraction of Fig.”
• Analytical approximations of K-corrections in optical and near-infrared bands (2010, methodology): “Mannucci et al. (2001) present in their fig.”