A Massive Z = 0.088 Supercluster and Tests of Starburst Galaxy Evolution at the North Ecliptic Pole

Ashby, M. L. N.; Hacking, P.; Houck, J. R.; Soifer, B. T.; Weisstein, Eric W.

doi:10.1086/176667

Cited by 29 publications

(72 citation statements)

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“…Its sample comprises 64 sources detected both at 60 µm (Hacking & Houck 1987) and at 15 µm (Aussel et al 2000), with redshifts measured by Ashby et al (1996). Xu fitted the result obtained (see its Table 2 and Fig.…”

Section: The 15 µM Luminosity Functionsupporting

confidence: 59%

“…Such a sample is deeper than previous estimates (Ashby et al 1996), showing a tail extending up to z = 0.375, almost 4 Gyr in look-back time.…”

Section: The Far-ir Propertiescontrasting

confidence: 50%

“…The first attempt to build up the 15 µm LF of a NEPR subsample was made by Xu (2000). However, he said that it must be considered as a preliminary work because: i) the sample of galaxies used is an incomplete sample; ii) there is a possible misidentification between the sources in the 60 µm redshift survey of Ashby et al (1996) and the 15 µm sources in his work (see della , for more details); and iii) the model used to interpret the data treated all IR galaxies as a single population.…”

Section: Introductionmentioning

confidence: 99%

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A multi-wavelength study of the IRAS Deep Survey galaxy sample

Mazzei

Valle

Bettoni

2006

A&A

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Context. The luminosity function (LF) is a basic tool in the study of galaxy evolution since it constrains galaxy formation models. The earliest LF estimates in the IR and far-IR spectral ranges seem to suggest strong evolution. Deeper samples are needed to confirm these predictions. We have a useful IR data set, which provides a direct link between IRAS and ISO surveys, and the forthcoming deeper Spitzer Space Telescope and Akari cosmological surveys, to address this issue. Aims. This data set allows us to derive the 60 µm local LF to sensitivity levels 10 times deeper than before, to investigate evolutionary effects up to a redshift of 0.37, and, using the 60/15 µm bi-variate method, to analyze the poorly known 15 µm local LF of galaxies. Methods. We exploited our ISOCAM observations of the IRAS Deep Survey (IDS) fields, to correct the 60 µm fluxes for confusion effects and observational biases. We find indications of a significant incompleteness of the IDS sample, still one of the deepest far-IR selected galaxy samples, below 80 mJy. We have reliable identifications and spectroscopic redshifts for 100% of a complete subsample comprising 56 sources with S (60 µm) > 80 mJy. Results. With our spectroscopic coverage we construct the 60 µm LF for a sample complete down to 80 mJy. This LF extends over three orders of magnitude in luminosity, from 9 up to more than 12 in log(L 60 /L ). Despite the fact that the redshift range of our sample exceeds z = 0.3, the V/V max test gives V/V max = 0.51 ± 0.06, consistent with a uniform distribution of sources. A more direct test, whereby the LF was measured in each of four different redshift intervals, does not point out any signature of evolution. On the other hand, the rest-frame 15 µm local LF we derive, extends up to log(L 15 /L ) = 12 and predicts 10 times more sources at log(L 15 /L ) = 11 than before.

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Section: The 15 µM Luminosity Functionsupporting

confidence: 59%

“…Such a sample is deeper than previous estimates (Ashby et al 1996), showing a tail extending up to z = 0.375, almost 4 Gyr in look-back time.…”

Section: The Far-ir Propertiescontrasting

confidence: 50%

Section: Introductionmentioning

confidence: 99%

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A multi-wavelength study of the IRAS Deep Survey galaxy sample

Mazzei

Valle

Bettoni

2006

A&A

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“…The NEPR supercluster (NEPSC) found by Ashby et al (1996) (see also Burg et al 1992) dominates the z-distribution between 0.08 and 0.09. Galaxy members of other expected clusters appear between 0.05 and 0.06, 0.07, and between 0.11 and 0.12.…”

Section: Emission Line Flux Measurementmentioning

confidence: 92%

A multiwavelength study of the IRAS Deep Survey galaxy sample

Bettoni

Mazzei

Valle

2012

A&A

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Context. The infrared deep sample (IDS), in the north ecliptical polar region (NEPR), is the first complete, far-IR selected sample, on which numerous studies of galaxy evolution are based. Such a sample allows direct investigation of the evolution of dusty galaxies up to a redshift of about 0.3, where the global star formation rate is known to evolve very fast. As discussed in previous papers, we performed optical and IR (ISOCAM, 15 μm,) follow-up of its galaxies and exploited our IR observations to correct the 60 μm fluxes for confusion effects and observational biases. In them we found indications of a significant incompleteness of IDS sample below S (60) 80 mJy. We constructed 15 μm and far-IR (60 μm) luminosity functions of a complete sample of 56 ISO/IRAS sources. Aims.Here we present and analyze the spectral classification of several galaxies in the IDS sample together with rotation curves which allow estimating the lower mass limits of a subsample of objects. Methods. We measured fluxes and intensity ratios of the emission lines in the visible region of the spectrum (λ4000−9000 Å) for 75 galaxy members. Moreover, for some of them (55%), the spectra obtained with the Keck II telescope have sufficient wavelength and spatial resolution to derive their rotation curve.Results. These galaxies turn out to be disk like systems, with a high fraction (∼50%) of interacting systems. The spectroscopic classification of 42 galaxies, using the emission-line ratio diagnostic diagrams, shows that the NEPR sample is predominantly composed of starburst galaxies (71%), while the fraction of AGNs (7%) and LINERs (21%) is small. The dynamical analysis allows us to estimate the lower mass limits of 39 galaxies. Conclusions. The rest-frame FIR luminosity distribution of these galaxies spans the same range as that of the FIR selected complete sample, i.e. three orders of magnitude, with the same mean value, log(L FIR ) = 10.2. This emphasizes that such galaxies represent FIR properties of the whole sample well. Moreover, their optical properties are typical of the sample itself since 62% of these belong to the 60 μm selected complete sample.

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“…One reason to probe bright objects is to study the number counts of extragalactic sources and their spectral shapes. In the far-infrared (FIR) the sources detected by these surveys are usually dominated by low-redshift galaxies with z < 0.1, as found by IRAS at 60 μm (Ashby et al 1996) but a few extreme objects like the lensed F10214 source (Rowan-Robinson et al 1991) also appear. However, the population in the radio band is dominated by synchrotron sources (in particular, blazars) at higher redshift (see de Zotti et al 2010, for a recent review).…”

Section: Introductionmentioning

confidence: 95%

Planckintermediate results

Collaboration¹,

Ade

Aghanim

et al. 2013

A&A

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We make use of the Planck all-sky survey to derive number counts and spectral indices of extragalactic sources -infrared and radio sources -from the Planck Early Release Compact Source Catalogue (ERCSC) at 100 to 857 GHz (3 mm to 350 μm). Three zones (deep, medium and shallow) of approximately homogeneous coverage are used to permit a clean and controlled correction for incompleteness, which was explicitly not done for the ERCSC, as it was aimed at providing lists of sources to be followed up. Our sample, prior to the 80% completeness cut, contains between 217 sources at 100 GHz and 1058 sources at 857 GHz over about 12 800 to 16 550 deg 2 (31 to 40% of the sky). After the 80% completeness cut, between 122 and 452 and sources remain, with flux densities above 0.3 and 1.9 Jy at 100 and 857 GHz. The sample so defined can be used for statistical analysis. Using the multi-frequency coverage of the Planck High Frequency Instrument, all the sources have been classified as either dust-dominated (infrared galaxies) or synchrotron-dominated (radio galaxies) on the basis of their spectral energy distributions (SED). Our sample is thus complete, flux-limited and color-selected to differentiate between the two populations. We find an approximately equal number of synchrotron and dusty sources between 217 and 353 GHz; at 353 GHz or higher (or 217 GHz and lower) frequencies, the number is dominated by dusty (synchrotron) sources, as expected. For most of the sources, the spectral indices are also derived. We provide for the first time counts of bright sources from 353 to 857 GHz and the contributions from dusty and synchrotron sources at all HFI frequencies in the key spectral range where these spectra are crossing. The observed counts are in the Euclidean regime. The number counts are compared to previously published data (from earlier Planck results, Herschel, BLAST, SCUBA, LABOCA, SPT, and ACT) and models taking into account both radio or infrared galaxies, and covering a large range of flux densities. We derive the multi-frequency Euclidean level -the plateau in the normalised differential counts at high flux-density -and compare it to WMAP, Spitzer and IRAS results. The submillimetre number counts are not well reproduced by current evolution models of dusty galaxies, whereas the millimetre part appears reasonably well fitted by the most recent model for synchrotron-dominated sources. Finally we provide estimates of the local luminosity density of dusty galaxies, providing the first such measurements at 545 and 857 GHz.Key words. cosmology: observations -surveys -galaxies: statistics -galaxies: evolution -galaxies: star formation -galaxies: active Appendices are available in electronic form at

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A Massive Z = 0.088 Supercluster and Tests of Starburst Galaxy Evolution at the North Ecliptic Pole

Cited by 29 publications

References 0 publications

A multi-wavelength study of the IRAS Deep Survey galaxy sample

A multi-wavelength study of the IRAS Deep Survey galaxy sample

A multiwavelength study of the IRAS Deep Survey galaxy sample

Planckintermediate results

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