Submillimetre photometry of 323 nearby galaxies from the<i>Herschel</i>Reference Survey

Ciesla, L.; Boselli, A.; Smith, M.; Bendo, G. J.; Cortese, Luca; Eales, Stephen Anthony; Bianchi, S.; Boquien, M.; Buat, V.; Davies, Jonathan Ivor; Pohlen, M.; Zibetti, S.; Baes, M.; Cooray, Asantha; Looze, I. De; Alighieri, S. di Serego; Galametz, M.; Gomez, Haley Louise; Lebouteiller, V.; Madden, S.; Pappalardo, C.; Rémy, Aurélie; Spinoglio, L.; Vaccari, M.; Auld, Robbie Richard; Clements, D. L.

doi:10.1051/0004-6361/201219216

Cited by 112 publications

(157 citation statements)

References 58 publications

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“…On the other hand, Spitzer and Herschel have now provided us with deep imaging observations of significant numbers of nearby edge-on spiral galaxies at various FIR/submm wavelengths (e.g. Bianchi & Xilouris 2011;Holwerda et al 2012;De Looze et al 2012a,b;Ciesla et al 2012;Verstappen et al 2012).…”

Section: Discussionmentioning

confidence: 99%

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

Geyter

Baes

Fritz

et al. 2013

A&A

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We present FitSKIRT, a method to efficiently fit radiative transfer models to UV/optical images of dusty galaxies. These images have the advantage that they have better spatial resolution compared to FIR/submm data. FitSKIRT uses the GAlib genetic algorithm library to optimize the output of the SKIRT Monte Carlo radiative transfer code. Genetic algorithms prove to be a valuable tool in handling the multi-dimensional search space as well as the noise induced by the random nature of the Monte Carlo radiative transfer code. FitSKIRT is tested on artificial images of a simulated edge-on spiral galaxy, where we gradually increase the number of fitted parameters. We find that we can recover all model parameters, even if all 11 model parameters are left unconstrained. Finally, we apply the FitSKIRT code to a V-band image of the edge-on spiral galaxy NGC 4013. This galaxy has been modeled previously by other authors using different combinations of radiative transfer codes and optimization methods. Given the different models and techniques and the complexity and degeneracies in the parameter space, we find reasonable agreement between the different models. We conclude that the FitSKIRT method allows comparison between different models and geometries in a quantitative manner and minimizes the need of human intervention and biasing. The high level of automation makes it an ideal tool to use on larger sets of observed data.

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Section: Discussionmentioning

confidence: 99%

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

Geyter

Baes

Fritz

et al. 2013

A&A

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“…The total uncertainty in each measurement is given by the sum of the quadrature of the calibration (σ cal ) and photometry (σ phot ) uncertainties. Ciesla et al (2012) show that the first dominates the uncertainties of point-like sources (galaxies with angular diameters less than 20 , 29 , and 37 at 250, 350, and 500 μm bands of SPIRE) and the second of the more extended sources. The parameter σ phot includes the instrumental error (1−2%), the confusion error due to background sources (see Nguyen et al 2010), and the error of the sky (given by σ sky = N pixel · σ sky,pix , where N pixel is the number of pixels in each aperture and σ sky,pix the sky error per pixel).…”

Section: The Datamentioning

confidence: 95%

Herschelobservations of Hickson compact groups of galaxies: Unveiling the properties of cold dust

Bitsakis

Charmandaris

Appleton

et al. 2014

A&A

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We present a Herschel far-infrared and sub-millimetre (sub-mm) study of a sample of 120 galaxies in 28 Hickson compact groups (HCGs). Fitting their UV to sub-mm spectral energy distributions with the model of da Cunha et al. (2008), we accurately estimate the dust masses, luminosities, and temperatures of the individual galaxies. We find that nearly half of the late-type galaxies in dynamically "old" groups, those with more than 25% of early-type members and redder UV-optical colours, also have significantly lower dustto-stellar mass ratios compared to those of actively star-forming galaxies of the same mass found both in HCGs and in the field. Examining their dust-to-gas mass ratios, we conclude that dust was stripped out of these systems as a result of the gravitational and hydrodynamic interactions, experienced owing to previous encounters with other group members. About 40% of the early-type galaxies (mostly lenticulars), in dynamically "old" groups, display dust properties similar to those of the UV-optical red late-type galaxies. Given their stellar masses, star formation rates, and UV-optical colours, we suggest that red late-type and dusty lenticular galaxies represent transition populations between blue star-forming disk galaxies and quiescent early-type ellipticals. On the other hand, both the complete absence of any correlation between the dust and stellar masses of the dusty ellipticals and their enhanced star formation activity, suggest the increase in their gas and dust content due to accretion and merging. Our deep Herschel observations also allow us to detect the presence of diffuse cold intragroup dust in 4 HCGs. We also find that the fraction of 250 μm emission that is located outside of the main bodies of both the red late-type galaxies and the dusty lenticulars is 15−20% of their integrated emission at this band. All these findings are consistent with an evolutionary scenario in which gas dissipation, shocks, and turbulence, in addition to tidal interactions, shape the evolution of galaxies in compact groups.

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“…Because of this, it is preferable to use the timeline data for performing photometry measurements through point-spread function (PSF) fitting down to a level of 30 mJy, as the timeline data preserves the surface brightness and positional information of each individual measurement (see also, Pearson et al 2013, and their tests with different methods). We also note that sourceExtractorSussextractor itself is subject to some systematic bias issues related to how it uses the error map for weighting (Smith et al 2012). …”

Section: Source Identification and Flux Density Measurementmentioning

confidence: 99%

“…To quantify the number of false detections due to the instrumental noise, we use a permutation method similar to that used by Smith et al (2012). We build two maps using the two halves of the eight HeViCS-scans and calculate two difference maps:…”

Section: Reliabilitymentioning

confidence: 99%

TheHerschelVirgo Cluster Survey

Pappalardo

Bendo

Bianchi

et al. 2015

A&A

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Aims. We present three independent catalogs of point-sources extracted from SPIRE images at 250, 350, and 500 µm, acquired with the Herschel Space Observatory as a part of the Herschel Virgo Cluster Survey (HeViCS). The catalogs have been cross-correlated to consistently extract the photometry at SPIRE wavelengths for each object. Methods. Sources have been detected using an iterative loop. The source positions are determined by estimating the likelihood to be a real source for each peak on the maps, according to the criterion defined in the sourceExtractorSussextractor task. The flux densities are estimated using the sourceExtractorTimeline, a timeline-based point source fitter that also determines the fitting procedure with the width of the Gaussian that best reproduces the source considered. Afterwards, each source is subtracted from the maps, removing a Gaussian function in every position with the full width half maximum equal to that estimated in sourceExtractorTimeline. This procedure improves the robustness of our algorithm in terms of source identification. We calculate the completeness and the flux accuracy by injecting artificial sources in the timeline and estimate the reliability of the catalog using a permutation method. Results. The HeViCS catalogs contain about 52 000, 42 200, and 18 700 sources selected at 250, 350, and 500 µm above 3σ and are ∼75%, 62%, and 50% complete at flux densities of 20 mJy at 250, 350, 500 µm, respectively. We then measured source number counts at 250, 350, and 500 µm and compare them with previous data and semi-analytical models. We also cross-correlated the catalogs with the Sloan Digital Sky Survey to investigate the redshift distribution of the nearby sources. From this crosscorrelation, we select ∼2000 sources with reliable fluxes and a high signal-to-noise ratio, finding an average redshift z ∼ 0.3 ± 0.22 and 0.25 (16-84 percentile). Conclusions. The number counts at 250, 350, and 500 µm show an increase in the slope below 200 mJy, indicating a strong evolution in number of density for galaxies at these fluxes. In general, models tend to overpredict the counts at brighter flux densities, underlying the importance of studying the Rayleigh-Jeans part of the spectral energy distribution to refine the theoretical recipes of the models. Our iterative method for source identification allowed the detection of a family of 500 µm sources that are not foreground objects belonging to Virgo and not found in other catalogs.

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Submillimetre photometry of 323 nearby galaxies from theHerschelReference Survey

Cited by 112 publications

References 58 publications

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

Herschelobservations of Hickson compact groups of galaxies: Unveiling the properties of cold dust

TheHerschelVirgo Cluster Survey

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