Erratum: “An Ultraviolet‐to‐Radio Broadband Spectral Atlas of Nearby Galaxies” (ApJ, 655, 863 [2007])

Dale, Daniel A.; Paz, A. Gil de; Hanson, Heather; Armus, L.; Bendo, G. J.; Bianchi, Luciana; Block, M.; Boissier, S.; Boselli, A.; Buckalew, B.; Buat, V.; Burgarella, D.; Calzetti, Daniela; Cannon, John; Engelbracht, C. W.; Hélou, G.; Hollenbach, D. J.; Jarrett, T. H.; Kennicutt, Robert C.; Leitherer, Claus; Li, A.; Madore, B. F.; Meyer, M.; Murphy, E. J.; Regan, Michael W.; Roussel, H.; Smith, John David; Sosey, M.; Thilker, David A.; Walter, Fabian

doi:10.1086/523847

Cited by 103 publications

(197 citation statements)

References 0 publications

Supporting

Mentioning

183

Contrasting

Unclassified

Order By: Relevance

“…Dale et al (2007Dale et al ( , 2008 published UV-to-radio broad-bands SEDs for the SINGS galaxies. The listed data comprises the FUV (∼1500 Å) and NUV (∼2300 Å) filters of GALEX , 2MASS data for J, H, and K s (Jarrett et al 2003), and IRAC and MIPS data for the filters centred on 3.…”

Section: Fig 11mentioning

confidence: 99%

“…Apart from all non-optical Dale et al filters up to MIPS 160 μm, their catalogue provides photometry of the Sloan Digital Sky Survey (SDSS; Stoughton et al 2002) in u , g , r , i , and z for 32 SINGS objects. Moreover, the Dale et al (2007Dale et al ( , 2008 optical magnitudes of 23 galaxies without SDSS photometry were recalibrated by means of the catalogue of Prugniel & Heraudeau (1998), i.e., their aperture photometry was replicated on the SINGS optical images to derive zero-point corrections for each filter and each galaxy. For our sample selection we have required either the presence of SDSS photometry or at least Fig.…”

Section: Fig 11mentioning

confidence: 99%

See 1 more Smart Citation

Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample

Noll

Burgarella

Giovannoli

et al. 2009

A&A

Self Cite

927

1,001

View full text Add to dashboard Cite

Aims. Photometric data of galaxies covering the rest-frame wavelength range from far-UV to far-IR make it possible to derive galaxy properties with a high reliability by fitting the attenuated stellar emission and the related dust emission at the same time.Methods. For this purpose we wrote the code CIGALE (Code Investigating GALaxy Emission) that uses model spectra composed of the Maraston (or PEGASE) stellar population models, synthetic attenuation functions based on a modified Calzetti law, spectral line templates, the Dale & Helou dust emission models, and optional spectral templates of obscured AGN. Depending on the input redshifts, filter fluxes were computed for the model set and compared to the galaxy photometry by carrying out a Bayesian-like analysis. CIGALE was tested by analysing 39 nearby galaxies selected from SINGS. The reliability of the different model parameters was evaluated by studying the resulting expectation values and their standard deviations in relation to the input model grid. Moreover, the influence of the filter set and the quality of photometric data on the code results was estimated. Results. For up to 17 filters with effective wavelengths between 0.15 and 160 μm, we find robust results for the mass, star formation rate, effective age of the stellar population at 4000 Å, bolometric luminosity, luminosity absorbed by dust, and attenuation in the far-UV. Details of the star formation history (excepting the burst fraction) and the shape of the attenuation curve are difficult to investigate with the available broad-band UV and optical photometric data. A study of the mutual relations between the reliable properties confirms the dependence of star formation activity on morphology in the local Universe and indicates a significant drop in this activity at about 10 11 M towards higher total stellar masses. The dustiest galaxies in the SINGS sample are present in the same mass range. On the other hand, the far-UV attenuation of our sample galaxies does not appear to show a significant dependence on star formation activity. Conclusions. The results for our SINGS test sample demonstrate that CIGALE can be a valuable tool for studying basic properties of galaxies in the near and distant Universe if UV-to-IR data are available.

show abstract

Section: Fig 11mentioning

confidence: 99%

Section: Fig 11mentioning

confidence: 99%

Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample

Noll

Burgarella

Giovannoli

et al. 2009

A&A

Self Cite

927

1,001

View full text Add to dashboard Cite

show abstract

“…Most regions in the KINGFISH sample were also included in the Spitzer Infrared Nearby Galaxies Survey (SINGS) (Kennicutt et al 2003;Dale et al 2006;Smith et al 2007b). This survey used the Spitzer Space Telescope to obtain infrared imaging and spectroscopy for 75 nearby galaxies.…”

Section: Ancillary Infrared Observationsmentioning

confidence: 99%

“…In most cases, the larger BtP maps were covered with Spitzer /IRS by only the LL module. All observations were reduced with the CUBISM program to create spatially resolved spectral cubes and processed using the IRS pipeline version S14 producing and absolute flux calibration uncertainty of ∼ 25% Dale et al (2006). For more information on these observations and data processing, see Smith et al (2007a).…”

Section: Ancillary Infrared Observationsmentioning

confidence: 99%

Using [C ii] 158 μm Emission from Isolated ISM Phases as a Star Formation Rate Indicator

Sutter

Dale

Croxall³

et al. 2019

ApJ

Self Cite

View full text Add to dashboard Cite

The brightest observed emission line in many star-forming galaxies is the [CII] 158 µm line, making it detectable up to z∼7. In order to better understand and quantify the [CII] emission as a tracer of star-formation, the theoretical ratio between the [NII] 205 µm emission and the [CII] 158 µm emission has been employed to empirically determine the fraction of [CII] emission that originates from the ionized and neutral phases of the ISM. Sub-kiloparsec measurements of the [CII] 158 µm and [NII] 205 µm line in nearby galaxies have recently become available as part of the Key Insights in Nearby Galaxies: a Far Infrared Survey with Herschel (KINGFISH) and Beyond the Peak (BtP) programs. With the information from these two far-infrared lines along with the multi-wavelength suite of KINGFISH data, a calibration of the [CII] emission line as a star formation rate indicator and a better understanding of the [CII] deficit are pursued.[CII] emission is also compared to PAH emission in these regions to compare photoelectric heating from PAH molecules to cooling by [CII] in the neutral and ionized phases of the ISM. We find that the [CII] emission originating in the neutral phase of the ISM does not exhibit a deficit with respect to the infrared luminosity and is therefore preferred over the [CII] emission originating in the ionized phase of the ISM as a star formation rate indicator for the normal star-forming galaxies included in this sample.

show abstract

“…Instead of collecting data from any available literature source, we restrict our selection to only a few well-documented, homogeneous compilations. For the ultraviolet, we select FUV (1350-1750 Å) and NUV (1750-2800 Å) measurements principally from the Galaxy Evolution Explorer (GALEX) atlases of Buat et al (2007), Dale et al (2007), and Gil de Paz et al (2007). At present, only ∼16% of our sample has published GALEX data, although the situation will soon improve substantially with the recent completion of the All-Sky Imaging Survey.…”

Section: Isophotal and Photometric Parameters Derived From Cgsmentioning

confidence: 99%

The Carnegie-Irvine Galaxy Survey. I. Overview and Atlas of Optical Images

Barth

et al. 2011

ApJS

165

186

View full text Add to dashboard Cite

The Carnegie-Irvine Galaxy Survey (CGS) is a long-term program to investigate the photometric and spectroscopic properties of a statistically complete sample of 605 bright (B T < 12.9 mag), southern (δ < 0• ) galaxies using the facilities at Las Campanas Observatory. This paper, the first in a series, outlines the scientific motivation of CGS, defines the sample, and describes the technical aspects of the optical broadband (BVRI) imaging component of the survey, including details of the observing program, data reduction procedures, and calibration strategy. The overall quality of the images is quite high, in terms of resolution (median seeing ∼1 ), field of view (8. 9 × 8. 9), and depth (median limiting surface brightness ∼27.5, 26.9, 26.4, and 25.3 mag arcsec −2 in the B, V, R, and I bands, respectively). We prepare a digital image atlas showing several different renditions of the data, including three-color composites, star-cleaned images, stacked images to enhance faint features, structure maps to highlight small-scale features, and color index maps suitable for studying the spatial variation of stellar content and dust. In anticipation of upcoming science analyses, we tabulate an extensive set of global properties for the galaxy sample. These include optical isophotal and photometric parameters derived from CGS itself, as well as published information on multiwavelength (ultraviolet, U-band, near-infrared, far-infrared) photometry, internal kinematics (central stellar velocity dispersions, disk rotational velocities), environment (distance to nearest neighbor, tidal parameter, group, or cluster membership), and H i content. The digital images and science-level data products will be made publicly accessible to the community.

show abstract

Erratum: “An Ultraviolet‐to‐Radio Broadband Spectral Atlas of Nearby Galaxies” (ApJ, 655, 863 [2007])

Cited by 103 publications

References 0 publications

Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample

Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample

Using [C ii] 158 μm Emission from Isolated ISM Phases as a Star Formation Rate Indicator

The Carnegie-Irvine Galaxy Survey. I. Overview and Atlas of Optical Images

Contact Info

Product

Resources

About