The XMM-SERVS survey: new XMM–Newton point-source catalogue for the XMM-LSS field

Chen, Chien-Ting; Brandt, W. N.; Luo, B.; Ranalli, P.; Yang, Guang; Alexander, D. M.; Bauer, F. E.; Kelson, Daniel D.; Lacy, Mark; Nyland, Kristina; Tozzi, P.; Vito, F.; Cirasuolo, M.; Gilli, R.; Jarvis, Matt J.; Lehmer, Bret; Paolillo, M.; Schneider, Donald P.; Shemmer, Ohad; Smail, Ian; Sun, Mouyuan; Tanaka, Masayuki; Vaccari, M.; Vignali, C.; Xue, Yongquan; Banerji, M.; Chow, Kate; Häußler, Boris; Norris, R. P.; Silverman, John D.; Trump, Jonathan R.

doi:10.1093/mnras/sty1036

Cited by 76 publications

(28 citation statements)

References 79 publications

(124 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A summary of the existing multiwavelength data used in this paper is listed in Table 3 (for details on the full set of multiwavelength data available, see Vaccari 2015). A more comprehensive overview of the ancillary optical and ground-based near-IR surveys with survey depths is also given in Mauduit et al (2012) and Chen et al (2018) as well as Table 3.…”

Section: Servs Data Fusion -Optical and Near-ir Photometrymentioning

confidence: 99%

Photometric redshifts for galaxies in the Spitzer Extragalactic Representative Volume Survey (SERVS)

Pforr

Vaccari

Lacy

et al. 2018

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present photometric redshifts for ∼4 million galaxies detected in the Spitzer 3.6 or 4.5 μm bands of the Spitzer Extragalactic Representative Volume Survey (SERVS). The 18 deg 2 area of SERVS covers five extragalactic fields with a variety of ancillary, optical, and near-infrared (IR) photometry. We evaluate the accuracy of our photometric redshifts with ∼90.000 publicly available, spectroscopic redshifts. Overall, we find an average of ∼0.038 for the normalized median absolute deviation (σ NMAD), a measure similar to the standard deviation yet more robust against outliers, and outlier fraction η of 3.7 per cent for the sources with the widest wavelength coverage. On the example of the XMM field, we quantify the quality and reliability of photometric redshifts as a function of (1) the number of photometric bands available in the fitting, (2) i AB magnitude, (3) Infrared Array Camera (IRAC) 3.6 μm magnitude, (4) spectroscopic redshift, and (5) the survey origin of the spectroscopic redshift. The best results are achieved when the photometry available for the fitting covers rest-frame optical and near-IR wavelengths. σ NMAD and η are smallest for the brightest objects. Similarly, we find σ NMAD and η to be smaller on average at z < 1.5 than at z > 1.5. Photometric redshifts derived without the two IRAC filter bands, but detections in all other bands are slightly underestimated. Approximately 76 per cent of SERVS sources with at least five available filter bands lie between redshift 0 and ∼1.5. We find a tail of high-redshift galaxies, i.e. ∼7 per cent of all objects with at least five available filter bands for the fitting lie at z > 3. We discuss ways to improve upon the photometric redshifts for SERVS galaxies in the future.

show abstract

Section: Servs Data Fusion -Optical and Near-ir Photometrymentioning

confidence: 99%

Photometric redshifts for galaxies in the Spitzer Extragalactic Representative Volume Survey (SERVS)

Pforr

Vaccari

Lacy

et al. 2018

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…In the future, we will further develop X-CIGALE and enable it to address special AGNs such as radio-loud and BAL objects ( §2.2). Besides the three surveys tested in this work (SDSS, COSMOS, and AKARI-NEP), the user can apply X-CIGALE to the existing multiwavelength surveys such as CDF-S (Luo et al 2017), CDF-N (Xue et al 2016), and XMM-SERVS (Chen et al 2018). In the future, X-CIGALE can be used to explore deep/wide surveys of, e.g.…”

Section: Summary and Future Prospectsmentioning

confidence: 99%

“…Considering these advantageous properties, X-ray observations are widely used to select AGNs, especially in the distant universe, (e.g. Luo et al 2017;Chen et al 2018). These selections are often more complete and reliable than the selections at other wavelengths such as optical and IR.…”

Section: Introductionmentioning

confidence: 99%

x-cigale: fitting AGN/galaxy SEDs from X-ray to infrared

Yang

Boquien

Buat

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

183

View full text Add to dashboard Cite

CIGALE is a powerful multiwavelength spectral energy distribution (SED) fitting code for extragalactic studies. However, the current version of CIGALE is not able to fit X-ray data, which often provide unique insights into AGN intrinsic power. We develop a new X-ray module for CIGALE, allowing it to fit SEDs from the X-ray to infrared (IR). We also improve the AGN fitting of CIGALE from UV-to-IR wavelengths. We implement a modern clumpy two-phase torus model, SKIRTOR. To account for moderately extincted type 1 AGNs, we implement polar-dust extinction. We publicly release the source code (named "X-CIGALE"). We test X-CIGALE with X-ray detected AGNs in SDSS, COSMOS, and AKARI-NEP. The fitting quality (as indicated by reduced χ 2 ) is good in general, indicating that X-CIGALE is capable of modelling the observed SED from X-ray to IR. We discuss constrainability and degeneracy of model parameters in the fitting of AKARI-NEP, for which excellent mid-IR photometric coverage is available. We also test fitting a sample of AKARI-NEP galaxies for which only X-ray upper limits are available from Chandra observations, and find that the upper limit can effectively constrain the AGN SED contribution for some systems. Finally, using X-CIGALE, we assess the ability of Athena to constrain the AGN activity in future extragalactic studies.

show abstract

“…Goulding et al 2017) based on wide surveys, e.g. XMM-XXL (Pierre et al 2016), Stripe 82X (LaMassa et al 2016), XMM-SERVS (Chen et al 2018), and the Chandra Source Catalog (Evans et al 2010). Compared to distant systems in deep fields, local sources have the advantages of larger sample sizes and more accurate morphological measurements, and these advantages could reduce the uncertainties of the BHAR-SFR relation significantly.…”

Section: S U M M a Ry A N D F U T U R E W O R Kmentioning

confidence: 99%

Evident black hole-bulge coevolution in the distant universe

Yang

Brandt

Alexander

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACT Observations in the local universe show a tight correlation between the masses of supermassive black holes (SMBHs; M BH ) and host-galaxy bulges (M bulge ), suggesting a strong connection between SMBH and bulge growth.However, direct evidence for such a connection in the distant universe remains elusive. We have studied sample-averaged SMBH accretion rate (BHAR) for bulge-dominated galaxies at z = 0.5-3. While previous observations found BHAR is strongly related to host-galaxy stellar mass (M ) for the overall galaxy population, our analyses show that, for the bulge-dominated population, BHAR is mainly related to SFR rather than M . This BHAR-SFR relation is highly significant, e.g. 9.0σ (Pearson statistic) at z = 0.5-1.5. Such a BHAR-SFR connection does not exist among our comparison sample of galaxies that are not bulge dominated, for which M appears to be the main determinant of SMBH accretion. This difference between the bulge-dominated and comparison samples indicates that SMBHs only coevolve with bulges rather than the entire galaxies, explaining the tightness of the local M BH −M bulge correlation. Our best-fitting BHAR-SFR relation for the bulge-dominated sample is log BHAR = log SFR − (2.48 ± 0.05) (solar units). The best-fitting BHAR/SFR ratio (10 −2.48 ) for bulge-dominated galaxies is similar to the observed M BH /M bulge values in the local universe. Our results reveal that SMBH and bulge growth are in lockstep, and thus non-causal scenarios of merger averaging are unlikely the origin of the M BH −M bulge correlation. This lockstep growth also predicts that the M BH −M bulge relation should not have strong redshift dependence.

show abstract

The XMM-SERVS survey: new XMM–Newton point-source catalogue for the XMM-LSS field

Cited by 76 publications

References 79 publications

Photometric redshifts for galaxies in the Spitzer Extragalactic Representative Volume Survey (SERVS)

Photometric redshifts for galaxies in the Spitzer Extragalactic Representative Volume Survey (SERVS)

x-cigale: fitting AGN/galaxy SEDs from X-ray to infrared

Evident black hole-bulge coevolution in the distant universe

Contact Info

Product

Resources

About