The NRAO VLA Sky Survey

Condon, J. J.; Cotton, W. D.; Greisen, E. W.; Yin, Qiang; Perley, R. A.; Taylor, G. B.; Broderick, J. J.

doi:10.1086/300337

Cited by 5,525 publications

(6,131 citation statements)

References 31 publications

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“…Although they do not exactly correspond to real data, some of their characteristics have been selected to resemble those from current surveys. For instance, the high-z survey can be representative of a radio survey like NVSS (Condon et al 1998), the one peaked at intermediate-z has a redshift distribution typical of luminous galaxies from SDSS (Ahn et al 2012) and, finally, the low-z survey includes near galaxies like the photometrically-selected galaxies from the SDSS (Aihara et al 2011). The different levels of noise have also been chosen to be similar to those of the three aforementioned surveys.…”

Section: Simulated Mapsmentioning

confidence: 99%

On the recovery of ISW fluctuations using large-scale structure tracers and CMB temperature and polarization anisotropies

Bonavera

Barreiro

Vielva

2016

Mon. Not. R. Astron. Soc.

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In this work we present a method to extract the signal induced by the integrated Sachs-Wolfe (ISW) effect in the cosmic microwave background (CMB). It makes use of the Linear Covariance-Based filter introduced by Barreiro et al., and combines CMB data with any number of large-scale structure (LSS) surveys and lensing information. It also exploits CMB polarization to reduce cosmic variance. The performance of the method has been thoroughly tested with simulations taking into account the impact of non-ideal conditions such as incomplete sky coverage or the presence of noise. In particular, three galaxy surveys are simulated, whose redshift distributions peak at low (z 0.3), intermediate (z 0.6) and high redshift (z 0.9). The contribution of each of the considered data sets as well as the effect of a mask and noise in the reconstructed ISW map is studied in detail. When combining all the considered data sets (CMB temperature and polarization, the three galaxy surveys and the lensing map), the proposed filter successfully reconstructs a map of the weak ISW signal, finding a perfect correlation with the input signal for the ideal case and around 80 per cent, on average, in the presence of noise and incomplete sky coverage. We find that including CMB polarization improves the correlation between input and reconstruction although only at a small level. Nonetheless, given the weakness of the ISW signal, even modest improvements can be of importance. In particular, in realistic situations, in which less information is available from the LSS tracers, the effect of including polarisation is larger. For instance, for the case in which the ISW signal is recovered from CMB plus only one survey, and taking into account the presence of noise and incomplete sky coverage, the improvement in the correlation coefficient can be as large as 10 per cent.

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Section: Simulated Mapsmentioning

confidence: 99%

On the recovery of ISW fluctuations using large-scale structure tracers and CMB temperature and polarization anisotropies

Bonavera

Barreiro

Vielva

2016

Mon. Not. R. Astron. Soc.

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“…Additionally, we can expect contributions to the 870 μm fluxes from radio continuum emission (synchrotron emission and/or bremsstrahlung). Three radio fluxes were estimated for Haro 11 with the NRAO VLA Sky Survey (8.46 and 1.4 GHz - Condon et al 1998) and the Sydney University Molonglo Sky Survey (843 MHz - Mauch et al 2003). We derive the 870 μm radio continuum contribution by extrapolation of the radio data tendancy (ν −1 ).…”

Section: Contamination Of the 870 μM Emission From Non-dust Originsmentioning

confidence: 99%

Probing the dust properties of galaxies up to submillimetre wavelengths

Galametz¹,

Madden²,

Galliano³

et al. 2009

A&A

100

200

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Aims. We study the dust properties of four low metallicity galaxies by modelling their spectral energy distributions. This modelling enables us to constrain the dust properties such as the mass, the temperature or the composition to characterise the global ISM properties in dwarf galaxies. Methods. We present 870 μm images of four low metallicity galaxies (NGC 1705, Haro 11, Mrk 1089 and UM 311) observed with the Large APEX BOlometer CAmera (LABOCA) on the Atacama Pathfinder EXperiment (APEX) telescope. We modeled their spectral energy distributions combining the submm observations of LABOCA, 2MASS, IRAS, Spitzer photometric data, and the IRS data for Haro 11. Results. We found that the PAH mass abundance is very low in these galaxies, 5 to 50 times lower than the PAH mass fraction of our Galaxy. We also found that a significant mass of dust is revealed when using submm constraints compared to that measured with only mid-IR to far-IR observations extending only to 160 μm. For NGC 1705 and Haro 11, an excess in submillimeter wavelengths was detected when we used our standard dust SED model. We rerun our SED procedure adding a cold dust component (10 K) to better describe the high 870 μm flux derived from LABOCA observations, which significantly improves the fit. We found that at least 70% of the dust mass of these two galaxies can reside in a cold dust component. We also showed that the subsequent dust-to-gas mass ratios, considering HI and CO observations, can be strikingly high for Haro 11 in comparison with what is usually expected for these low-metallicity environments. Furthermore, we derived the star formation rate of our galaxies and compared them to the Schmidt law. Haro 11 falls anomalously far from the Schmidt relation. These results may suggest that a reservoir of hidden gas could be present in molecular form not traced by the current CO observations. While there can be a significant cold dust mass found in Haro 11, the SED peaks at exceptionally short wavelengths (36 μm), also highlighting the importance of the much warmer dust component heated by the massive star clusters in Haro 11. We also derived the total IR luminosities derived from our models and compared them with relations that derive this luminosity from Spitzer bands. We found that the Draine & Li (2007) formula compares well to our direct IR determinations.

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“…(iii) Hard X-ray background: The 2-8 keV HEAO map has excellent sky coverage and perhaps the best-constrained dipole [37], but the redshift distribution is poorly known and the estimated bias is small and may be consistent with b = 1 [38], so it is not known how sensitive this is to ∇σ 8 . (iv) Radio sources: The NRAO VLA Sky Survey [39] sample has been used to probe the moderate redshift range z ∼ 1, but its redshift distribution is still under debate [40,41,36]. More importantly the maps exhibit declination-dependent striping which is almost certainly a systematic artifact and precludes determination of the dipole [42].…”

Section: Choice Of Datasetmentioning

confidence: 99%

Constraints on cosmic hemispherical power anomalies from quasars

Hirata¹

2009

J. Cosmol. Astropart. Phys.

109

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Abstract. Recent analyses of the cosmic microwave background (CMB) maps from the WMAP satellite have uncovered evidence for a hemispherical power anomaly, i.e. a dipole modulation of the CMB power spectrum at large angular scales with an amplitude of ±14 percent. Erickcek et al have put forward an inflationary model to explain this anomaly. Their scenario is a variation on the curvaton scenario in which the curvaton possesses a large-scale spatial gradient that modulates the amplitude of CMB fluctuations. We show that this scenario would also lead to a spatial gradient in the amplitude of perturbations σ 8 , and hence to a dipole asymmetry in any highly biased tracer of the underlying density field. Using the high-redshift quasars from the Sloan Digital Sky Survey, we find an upper limit on such a gradient of |∇σ 8 |/σ 8 < 0.027r −1 lss (99% posterior probability), where r lss is the comoving distance to the last-scattering surface. This rules out the simplest version of the curvaton spatial gradient scenario.

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The NRAO VLA Sky Survey

Cited by 5,525 publications

References 31 publications

On the recovery of ISW fluctuations using large-scale structure tracers and CMB temperature and polarization anisotropies

On the recovery of ISW fluctuations using large-scale structure tracers and CMB temperature and polarization anisotropies

Probing the dust properties of galaxies up to submillimetre wavelengths

Constraints on cosmic hemispherical power anomalies from quasars

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