Exploring the relationship between black hole accretion and star formation with blind mid-/far-infrared spectroscopic surveys

Bonato, M.; Negrello, M.; Cai, Zhen-Yi; Zotti, G. de; Bressan, A.; Lapi, A.; Pozzi, F.; Gruppioni, C.; Danese, L.

doi:10.1093/mnras/stu1657

Cited by 9 publications

(29 citation statements)

References 66 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In this paper, we adopt the Cai et al (2013) evolutionary model, as upgraded by Bonato et al (2014b). The model was validated by comparison with a broad array of data: multi-frequency (optical, near-IR, mid-IR, FIR, sub-mm) luminosity functions of galaxies and AGNs at all available redshifts, multi-frequency redshift distributions at several flux density limits, multi-frequency source counts, global and per-redshift slices (Cai et al, 2013;Bonato et al, 2014a) 3 .…”

Section: Introductionmentioning

confidence: 99%

Origins Space Telescope: Predictions for far-IR spectroscopic surveys

Bonato

Zotti

Leisawitz

et al. 2019

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

We illustrate the extraordinary potential of the (far-IR) Origins Survey Spectrometer (OSS) on board the Origins Space Telescope (OST) to address a variety of open issues on the co-evolution of galaxies and AGNs. We present predictions for blind surveys, each of 1000 h, with different mapped areas (a shallow survey covering an area of 10 deg 2 and a deep survey of 1 deg 2 ) and two different concepts of the OST/OSS: with a 5.9 m telescope (Concept 2, our reference configuration) and with a 9.1 m telescope (Concept 1, previous configuration). In 1000 h, surveys with the reference concept will detect from ∼ 1.9 × 10 6 to ∼ 8.7 × 10 6 lines from ∼ 4.8 × 10 5 -2.7 × 10 6 star-forming galaxies and from ∼ 1.4 × 10 4 to ∼ 3.8 × 10 4 lines from ∼ 1.3 × 10 4 -3.5 × 10 4 AGNs. The shallow survey will detect substantially more sources than the deep one; the advantage of the latter in pushing detections to lower luminosities/higher redshifts turns out to be quite limited. The OST/OSS will reach, in the same observing time, line fluxes more than one order of magnitude fainter than the SPICA/SMI and will cover a much broader redshift range. In particular it will detect tens of thousands of galaxies at z ≥ 5, beyond the reach of that instrument. The polycyclic aromatic hydrocarbons lines are potentially bright enough to allow the detection of hundreds of thousands of star-forming galaxies up to z ∼ 8.5, i.e. all the way through the re-ionization epoch. The proposed surveys will allow us to explore the galaxy-AGN co-evolution up to z ∼ 5.5 − 6 with very good statistics. OST Concept 1 does not offer significant advantages for the scientific goals presented here.

show abstract

Section: Introductionmentioning

confidence: 99%

Origins Space Telescope: Predictions for far-IR spectroscopic surveys

Bonato

Zotti

Leisawitz

et al. 2019

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

show abstract

“…In the analysis performed in this work, we have considered the two PAH features at 6.2 and 11.25 µm and several mid-and far-IR fine-structure lines, including four emission lines from photodissociation regions, PDRs ([Si II] In Spinoglio et al (2012) "global" relations between the luminosity of the above lines and the total IR luminosity were derived for all the sources of the 12-µm selected sample of Seyfert galaxies (12MGS; Rush et al 1993), regardless the AGN type and the fraction of AGN contributing to the IR luminosity, while in Bonato et al (2014b) an attempt was made to correlate the line luminosity with the SF IR luminosity and the AGN bolometric luminosity, although the latter was derived using just a few representative SED templates, normalised to the observed 12µm flux density.…”

Section: Introductionmentioning

confidence: 99%

Tracing black hole accretion with SED decomposition and IR lines: from local galaxies to the high-zUniverse

Gruppioni

Berta

Spinoglio

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

116

View full text Add to dashboard Cite

We present new estimates of AGN accretion and star-formation luminosity in galaxies obtained for the local 12 µm sample of Seyfert galaxies (12MGS), by performing a detailed broad-band spectral energy distribution (SED) decomposition including the emission of stars, dust heated by star formation and a possible AGN dusty torus. Thanks to the availability of data from the X-rays to the sub-millimetre, we constrain and test the contribution of the stellar, AGN and star-formation components to the SEDs. The availability of Spitzer-IRS low resolution mid-infrared (mid-IR) spectra is crucial to constrain the dusty torus component at its peak wavelengths. The results of SED-fitting are also tested against the available information in other bands: the reconstructed AGN bolometric luminosity is compared to those derived from X-rays and from the high excitation IR lines tracing AGN activity like [Ne V] and [O IV]. The IR luminosity due to star-formation (SF) and the intrinsic AGN bolometric luminosity are shown to be strongly related to the IR line luminosity. Variations of these relations with different AGN fractions are investigated, showing that the relation dispersions are mainly due to different AGN relative contribution within the galaxy. Extrapolating these local relations between line and SF or AGN luminosities to higher redshifts, by means of recent Herschel galaxy evolution results, we then obtain mid-and far-IR line luminosity functions useful to estimate how many star-forming galaxies and AGN we expect to detect in the different lines at different redshifts and luminosities with future IR facilities (e.g., JWST, SPICA).

show abstract

“…In this paper we build upon earlier works in Bonato et al (2014aBonato et al ( , 2014bBonato et al ( , 2015 that include relations for line to total IR luminosity for a large number of SF and AGN mid-IR spectral lines. With these, we make specific predictions for the detectability of said lines in different redshift and IR luminosity regimes.…”

Section: Discussionmentioning

confidence: 99%

“…We used the calibrations derived by Bonato et al (2014aBonato et al ( , 2014bBonato et al ( , 2015 for 33 MIR fine-structure lines (placed in the rest-frame wavelength range 3.03λ25.98 μm); 4 PAH lines at 6.2, 7.7, 8.6 and 11.3 μm; and 2 silicate bands (in emission and in absorption) at 9.7 and 18.0 μm.…”

Section: Correlations Between Continuum and Line Luminositymentioning

confidence: 99%

“…The 33 MIR fine-structure lines are the following: Bonato et al (2014aBonato et al ( , 2014bBonato et al ( , 2015 on the basis of observations collected from the literature. For all the other lines with either insufficient or missing data, the line-to-continuum luminosity relations were derived in Bonato et al (2015) using the IDL Tool for Emission-line Ratio Analysis (ITERA) written by Brent Groves. 17 ITERA makes use of the library of published photoionization and shock models for line emission of astrophysical plasmas produced by the Modelling And Prediction in PhotoIonised Nebulae and Gasdynamical Shocks (MAPPINGS III) code.…”

Section: Correlations Between Continuum and Line Luminositymentioning

confidence: 99%

See 1 more Smart Citation

Exploring the Evolution of Star Formation and Dwarf Galaxy Properties with JWST/MIRI Serendipitous Spectroscopic Surveys

Bonato

Sajina

Zotti

et al. 2017

ApJ

View full text Add to dashboard Cite

The James Webb Space Telescope's Medium Resolution Spectrometer (MRS), will offer nearly two orders of magnitude improvement in sensitivity and >3× improvement in spectral resolution over our previous space-based mid-IR spectrometer, the Spitzer IRS. In this paper, we make predictions for spectroscopic pointed observations and serendipitous detections with the MRS. Specifically, pointed observations of Herschel sources require only a few minutes on source integration for detections of several star-forming and active galactic nucleus lines, out to z=3 and beyond. But the same data will also include tens of serendipitous 0z4 galaxies per field with infrared luminosities ranging ∼10 6 -10 13 L ☉ . In particular, for the first time and for free we will be able to explore the L IR <10 9 L ☉ regime out to z∼3. We estimate that with ∼ 100 such fields, statistics of these detections will be sufficient to constrain the evolution of the low-L end of the infrared luminosity function, and hence the star formation rate function. The above conclusions hold for a wide range in the potential low-L end of the IR luminosity function, and account for the PAH deficit in low-L, low-metallicity galaxies.

show abstract

Exploring the relationship between black hole accretion and star formation with blind mid-/far-infrared spectroscopic surveys

Cited by 9 publications

References 66 publications

Origins Space Telescope: Predictions for far-IR spectroscopic surveys

Origins Space Telescope: Predictions for far-IR spectroscopic surveys

Tracing black hole accretion with SED decomposition and IR lines: from local galaxies to the high-zUniverse

Exploring the Evolution of Star Formation and Dwarf Galaxy Properties with JWST/MIRI Serendipitous Spectroscopic Surveys

Contact Info

Product

Resources

About