The evolution of the dust temperatures of galaxies in the SFR–M∗plane up toz ~ 2

Magnelli, B.; Lutz, D.; Saintonge, A.; Berta, S.; Santini, P.; Symeonidis, M.; Altiéri, B.; Andreani, P.; Aussel, H.; Béthermin, M.; Bock, J. J.; Bongiovanni, Á.; Cepa, J.; Cimatti, A.; Conley, A.; Daddi, E.; Elbaz, D.; Schreiber, N. M. Förster; Genzel, R.; Ivison, R. J.; Floc’h, E. Le; Magdis, G.; Maiolino, R.; Nordon, R.; Oliver, S.; Page, M. J.; García, A.; Poglitsch, A.; Popesso, P.; Pozzi, F.; Riguccini, L.; Rodighiero, G.; Rosario, D. J.; Roseboom, I. G.; Sánchez‐Portal, M.; Scott, D.; Sturm, E.; Tacconi, L. J.; Valtchanov, I.; Wang, L.; Wuyts, Stijn

doi:10.1051/0004-6361/201322217

Cited by 253 publications

(438 citation statements)

References 93 publications

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“…These issues have been discussed and studied in Magnelli et al (2014). They found that in the GOODS-S, GOODS-N and COSMOS fields our multi-wavelength catalogues are complete for starforming galaxies with M * > 10 10 M up to z ∼ 2.…”

Section: Final Samplementioning

confidence: 98%

“…From the best-fitting DH SED template we also estimated T dust using the pairing between dust temperature and DH templates established in Magnelli et al (2014). The reliability of these dust temperature estimates depends on the number of FIR data points available and on whether those data points encompass the peak of the FIR emission.…”

Section: Determination Of Far-infrared Properties Through Stackingmentioning

confidence: 99%

“…The reliability of these dust temperature estimates depends on the number of FIR data points available and on whether those data points encompass the peak of the FIR emission. As in Magnelli et al (2014), we considered as reliable only the dust temperatures inferred from at least three FIR data points encompassing the peak of the FIR emission and with χ 2 reduced < 3.…”

Section: Determination Of Far-infrared Properties Through Stackingmentioning

confidence: 99%

“…morphology, CO-to-H 2 conversion factor, dust temperature) of star-forming galaxies vary with their positions in the SFR-M * plane (e.g. Wuyts et al 2011b;Magnelli et al 2012bMagnelli et al , 2014. In particular, these properties correlate with the distance of a galaxy to the so-called main sequence (MS) of the SFR-M * plane, i.e.…”

Section: Introductionmentioning

confidence: 99%

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The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M_∗plane up toz~2

Magnelli

Ivison

Lutz

et al. 2014

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We study the evolution of the radio spectral index and far-infrared/radio correlation (FRC) across the star-formation rate -stellar masse (i.e. SFR-M * ) plane up to z ∼ 2. We start from a stellar-mass-selected sample of galaxies with reliable SFR and redshift estimates. We then grid the SFR-M * plane in several redshift ranges and measure the infrared luminosity, radio luminosity, radio spectral index, and ultimately the FRC index (i.e. q FIR ) of each SFR-M * -z bin. The infrared luminosities of our SFR-M * -z bins are estimated using their stacked far-infrared flux densities inferred from observations obtained with the Herschel Space Observatory. Their radio luminosities and radio spectral indices (i.e. α, where S ν ∝ ν −α ) are estimated using their stacked 1.4 GHz and 610 MHz flux densities from the Very Large Array and Giant Metre-wave Radio Telescope, respectively. Our far-infrared and radio observations include the most widely studied blank extragalactic fields -GOODS-N, GOODS-S, ECDFS, and COSMOS -covering a total sky area of ∼2.0 deg 2 . Using this methodology, we constrain the radio spectral index and FRC index of star-forming galaxies with M * > 10 10 M and 0 < z < 2.3. We find that α 1.4 GHz 610 MHz does not evolve significantly with redshift or with the distance of a galaxy with respect to the main sequence (MS) of the SFR-M * plane (i.e. Δlog(SSFR) MS = log[SSFR(galaxy)/SSFR MS (M * , z)]). Instead, star-forming galaxies have a radio spectral index consistent with a canonical value of 0.8, which suggests that their radio spectra are dominated by non-thermal optically thin synchrotron emission. We find that the FRC index, q FIR , displays a moderate but statistically significant redshift evolution as q FIR (z) = (2.35±0.08)×(1+z) −0.12 ± 0.04 , consistent with some previous literature. Finally, we find no significant correlation between q FIR and Δlog(SSFR) MS , though a weak positive trend, as observed in one of our redshift bins (i.e. Δ[q FIR ]/Δ[Δlog(SSFR) MS ] = 0.22 ± 0.07 at 0.5 < z < 0.8), cannot be firmly ruled out using our dataset.

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Section: Final Samplementioning

confidence: 98%

Section: Determination Of Far-infrared Properties Through Stackingmentioning

confidence: 99%

Section: Determination Of Far-infrared Properties Through Stackingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M_∗plane up toz~2

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Ivison

Lutz

et al. 2014

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“…There is a substantial amount of observational evidence that suggests a redshift evolution of the total IR luminosity and dust temperature (e.g. Amblard et al 2010;Elbaz et al 2010;Hwang et al 2010;Casey et al 2012;Magnelli et al 2014).…”

Section: Number Countsmentioning

confidence: 99%

TheHerschelVirgo Cluster Survey

Pappalardo

Bendo

Bianchi

et al. 2015

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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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Galactic Bulges

2016

Astrophysics and Space Science Library

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978-3-319-19377-9 ISBN 978-3-319-19378-6 (eBook) DOI 10.1007/978-3-319-19378-6 Library of Congress Control Number: 2015949217 Springer Cham Heidelberg New York Dordrecht London © Springer International Publishing Switzerland 2016 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors or omissions that may have been made.Cover Illustration: In the cover the 3.6 images of one nearby galaxy, NGC 4565, is shown. The images are from the Spitzer Survey of Stellar Structure in Galaxies (PI Kartik Sheth).Printed on acid-free paper Springer International Publishing AG Switzerland is part of Springer Science+Business Media (www.springer.com) PrefaceThe main motivation for this book was our impression that when observers talk about bulges in galaxies, they do not necessarily mean the same thing as people making theoretical models. Even among the observers, it is not always clear what they mean by classical and pseudobulges. According to most researchers, classical bulges are highly relaxed systems typically formed in galaxy mergers or by coalescence of massive gas clumps at high redshifts, whereas pseudobulges have more disc-like properties. Some people divide pseudobulges further into discy pseudobulges, defined as small central discs in the plane of the galactic disc, and boxy/peanut bulges which are actually dynamically heated, vertically thick inner parts of bars. Galaxies can also have central star clusters, usually called nuclear clusters, which structures are not called bulges in this book (see the review by Cole and Debattista). In recent years significant progress has been made both on the theoretical and observational sides, including galactic and extragalactic research. In this book we try to bring all these communities closer to each other.Most probably many of us share the Copernican approach trying to understand the universe with some simple beautiful theory. Such an attempt is the current paradigm of structure formation, i.e., the hierarchical growth of dark matter halos ( CDM), and the subsequent formatio...

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The evolution of the dust temperatures of galaxies in the SFR–M_∗plane up toz ~ 2

Cited by 253 publications

References 93 publications

The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M_∗plane up toz~2

The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M_∗plane up toz~2

TheHerschelVirgo Cluster Survey

Galactic Bulges

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The evolution of the dust temperatures of galaxies in the SFR–M∗plane up toz ~ 2

Cited by 253 publications

References 93 publications

The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M∗plane up toz~2

The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M∗plane up toz~2

TheHerschelVirgo Cluster Survey

Galactic Bulges

Contact Info

Product

Resources

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The evolution of the dust temperatures of galaxies in the SFR–M_∗plane up toz ~ 2

The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M_∗plane up toz~2

The far-infrared/radio correlation and radio spectral index of galaxies in the SFR–M_∗plane up toz~2