Issue |
A&A
Volume 518, July-August 2010
Herschel: the first science highlights
|
|
---|---|---|
Article Number | L31 | |
Number of page(s) | 5 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361/201014552 | |
Published online | 16 July 2010 |
Herschel: the first science highlights
LETTER TO THE EDITOR
The far-infrared/radio correlation as probed by
Herschel![[*]](/icons/foot_motif.png)
R. J. Ivison1,2 - B. Magnelli3 - E. Ibar1 - P. Andreani4,5 - D. Elbaz6 - B. Altieri7 - A. Amblard8 - V. Arumugam2 - R. Auld9 - H. Aussel6 - T. Babbedge10 - S. Berta3 - A. Blain11 - J. Bock11,12 - A. Bongiovanni13 - A. Boselli14 - V. Buat14 - D. Burgarella14 - N. Castro-Rodríguez13 - A. Cava13 - J. Cepa13 - P. Chanial10 - A. Cimatti15 - M. Cirasuolo1 - D. L. Clements10 - A. Conley16 - L. Conversi7 - A. Cooray8,11 - E. Daddi6 - H. Dominguez17 - C. D. Dowell11,12 - E. Dwek18 - S. Eales9 - D. Farrah19 - N. Förster Schreiber3 - M. Fox10 - A. Franceschini20 - W. Gear9 - R. Genzel3 - J. Glenn16 - M. Griffin9 - C. Gruppioni21 - M. Halpern22 - E. Hatziminaoglou4 - K. Isaak9 - G. Lagache23 - L. Levenson11,12 - N. Lu11,24 - D. Lutz3 - S. Madden6 - B. Maffei25 - G. Magdis6 - G. Mainetti20 - R. Maiolino17 - L. Marchetti20 - G. E. Morrison26,27 - A. M. J. Mortier10 - H. T. Nguyen11,12 - R. Nordon3 - B. O'Halloran10 - S. J. Oliver19 - A. Omont28 - F. N. Owen29 - M. J. Page30 - P. Panuzzo6 - A. Papageorgiou9 - C. P. Pearson31,32 - I. Pérez-Fournon13 - A. M. Pérez García13 - A. Poglitsch3 - M. Pohlen9 - P. Popesso3 - F. Pozzi21 - J. I. Rawlings30 - G. Raymond9 - D. Rigopoulou31,33 - L. Riguccini6 - D. Rizzo10 - G. Rodighiero20 - I. G. Roseboom19 - M. Rowan-Robinson10 - A. Saintonge3 - M. Sanchez Portal7 - P. Santini17 - B. Schulz11,24 - D. Scott22 - N. Seymour30 - L. Shao3 - D. L. Shupe11,24 - A. J. Smith19 - J. A. Stevens34 - E. Sturm3 - M. Symeonidis30 - L. Tacconi3 - M. Trichas10 - K. E. Tugwell30 - M. Vaccari20 - I. Valtchanov7 - J. Vieira11 - L. Vigroux28 - L. Wang19 - R. Ward19 - G. Wright1 - C. K. Xu11,24 - M. Zemcov11,12
1 - UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
2 - Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
3 - Max-Planck-Institut für Extraterrestrische Physik (MPE), Postfach 1312, 85741, Garching, Germany
4 - ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
5 - INAF - Osservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste, Italy
6 - Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université
Paris Diderot, CE-Saclay, pt courrier 131, 91191 Gif-sur-Yvette, France
7 - Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, 28691 Madrid, Spain
8 - Department of Physics & Astronomy, University of California, Irvine, CA 92697, USA
9 - Cardiff School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK
10 - Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK
11 - California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USA
12 - Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
13 - Instituto de Astrofísica de Canarias (IAC) and Departamento de
Astrofísica, Universidad de La Laguna (ULL), La Laguna, Tenerife, Spain
14 - Laboratoire d'Astrophysique de Marseille, OAMP, Université
Aix-marseille, CNRS, 38 rue Frédéric Joliot-Curie, 13388 Marseille
cedex 13, France
15 - Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, 40127 Bologna, Italy
16 - Department of Astrophysical and Planetary Sciences, CASA 389-UCB, University of Colorado, Boulder, CO 80309, USA
17 - INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy
18 - Observational Cosmology Laboratory, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
19 - Astronomy Centre, Department of Physics & Astronomy, University of Sussex, Brighton BN1 9QH, UK
20 - Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, 3, 35122 Padova, Italy
21 - INAF - Osservatorio Astronomico di Roma, via di Franscati 33, 00040 Monte Porzio Catone, Italy
22 - Department of Physics and Astronomy, University of British
Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada
23 - Institut d'Astrophysique Spatiale (IAS), bâtiment 121, Université Paris-Sud 11 and CNRS (UMR 8617), 91405 Orsay, France
24 - Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, JPL, Pasadena, CA 91125, USA
25 - School of Physics and Astronomy, The University of Manchester, Alan Turing Building, Oxford Road, Manchester M13 9PL, UK
26 - Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA
27 - Canada-France-Hawaii Telescope, Kamuela, HI, 96743, USA
28 - Institut d'Astrophysique de Paris, UMR 7095, CNRS, UPMC Univ. Paris 06, 98bis boulevard Arago, 75014 Paris, France
29 - National Radio Astronomy Observatory, PO Box O, Socorro NM 87801, USA
30 - Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
31 - Space Science and Technology Department, Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK
32 - Institute for Space Imaging Science, University of Lethbridge, Lethbridge, Alberta T1K 3M4, Canada
33 - Astrophysics, Oxford University, Keble Road, Oxford OX1 3RH, UK
34 - Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Hertfordshire AL10 9AB, UK
Received 30 March 2010 / Accepted 23 April 2010
Abstract
We set out to determine the ratio,
,
of rest-frame
8-1000-
m flux,
,
to monochromatic radio flux, 1.4, for
galaxies selected at far-infrared (IR) and radio wavelengths, to
search for signs that the ratio evolves with redshift, luminosity or
dust temperature,
,
and to identify any far-IR-bright outliers -
useful laboratories for exploring why the far-IR/radio correlation
(FIRRC) is generally so tight when the prevailing theory suggests
variations are almost inevitable. We use flux-limited 250-
m and
1.4-GHz samples, obtained using Herschel and the Very Large Array
(VLA) in GOODS-North (-N). We determine bolometric IR output
using ten bands spanning
m,
exploiting data from PACS and SPIRE (PEP; HerMES), as well as Spitzer, SCUBA, AzTEC and MAMBO. We also explore the properties of an
-matched sample, designed to reveal evolution of
with
redshift, spanning log
= 11-12
and z=0-2, by
stacking into the radio and far-IR images. For 1.4-GHz-selected
galaxies in GOODS-N, we see tentative evidence of a break in the flux
ratio,
,
at
1.4
W Hz-1, where active
galactic nuclei (AGN) are starting to dominate the radio power
density, and of weaker correlations with redshift and
.
From our
250-
m-selected sample we identify a small number of far-IR-bright
outliers, and see trends of
with
1.4,
,
and redshift,
noting that some of these are inter-related. For our
-matched
sample, there is no evidence that
changes significantly as we
move back into the epoch of galaxy formation: we find
,
where
at z=0-2; however,
discounting the least reliable data at z<0.5 we find
,
modest evolution which may be related to the radio
background seen by ARCADE 2, perhaps driven by <10-
Jy radio
activity amongst ordinary star-forming galaxies at z>1.
Key words: galaxies: evolution - galaxies: starburst - infrared: galaxies - submillimeter: galaxies - radio continuum: galaxies
1 Introduction
For samples of local galaxies - on galactic and 100-pc scales
- there is a good correlation between far-IR and radio emission
(Helou et al. 1985; de Jong et al. 1985; Condon et al. 1991; Yun et al. 2001). The correlation spans many
orders of magnitude in luminosity, gas surface density and photon,
cosmic-ray and magnetic energy density, and arises because the far-IR
and radio wavelength regimes share a common link with luminous,
massive stars and their end products - dust, supernovae (SNe) and
cosmic rays. In the simplest models (dubbed ``calorimetry'' -
e.g. Lisenfeld et al. 1996; Voelk 1989), dust absorbs all of the ultraviolet radiation
from massive stars, re-radiating this energy in the far-IR, and when
those massive stars explode as SNe they generate cosmic-ray electrons
which lose all their energy in the radio regime, mainly via
synchrotron emission. A balance is thereby achieved between far-IR and
radio emission, assuming that the starburst timescale is sufficiently
long (>107 yr).
Traditionally,
and
are both employed to determine
star-formation rates, and the far-IR/radio flux density ratio has been
useful when estimating the redshift or
of a distant starburst, or
when defining samples of AGN (Bell 2003; Chapman et al. 2005; Donley et al. 2005; Ivison et al. 2002; Condon 1992; Carilli & Yun 1999), or probing magnetic field strength
(Thompson et al. 2006). For these reasons, and because of recent
observational advances at both far-IR and radio wavelengths, there has
been a deluge of FIRRC-related work recently, exploring why the
correlation exists and whether it continues to hold at progressively
larger look-back times (Ibar et al. 2008; Seymour et al. 2009; Ivison et al. 2010; Sargent et al. 2010a; Appleton et al. 2004; Garrett 2002). Prevailing theory
(e.g. Lacki et al. 2010) suggests that variations in the far-IR/radio
flux ratio should be virtually unavoidable and that the FIRRC thus
arises due to a mysterious combination of effects involving
bremsstrahlung, inverse Compton cooling, ionisation and the relative
fractions of primary/secondary cosmic-ray electrons/protons, as well
as the critical synchrotron frequency.
Aside from the modelling work of Lacki et al., recent advances
in this field have included the use of luminosity-matched samples
(between high and low redshift) to better probe evolution with
look-back time (Sargent et al. 2010b) and the use of measurements spanning
the far-IR and radio wavebands to avoid assumptions relating to kcorrections (Ivison et al. 2010), although Calzetti et al. (2010) have argued
that bands beyond 24 m contain a contribution from dust heated
by stars from previous episodes of star formation and so we might not
necessarily expect the correlation to improve. In this paper we
introduce flux-limited 250-
m- and 1.4-GHz-selected samples of
galaxies from Herschel and the VLA, as well as a luminosity-matched
sample selected at 24
m, spanning z=0-2, and determine their
spectral energy distributions (SEDs) spanning the entire far-IR
spectral region. We then investigate the FIRRC from the perspectives
of the 24-, 250-
m- and radio-selected samples.
2 Sample selection and data analysis
In this paper we present results from observations with Herschel (Pilbratt et al. 2010). The SPIRE instrument, its in-orbit performance, and its scientific capabilities are described by Griffin et al. (2010), and the SPIRE astronomical calibration methods and accuracy are outlined in Swinyard et al. (2010). PACS is described by Poglitsch et al. (2010).
Our datasets are drawn from the common area observed by PACS and SPIRE
at 100, 160, 250, 350 and 500 m as part of HerMES
(Oliver et al., in prep.) and PEP (Lutz et
al., in prep.) in the GOODS-N field, prior to acquisition of
data for GOODS-Herschel. GOODS-N has also been observed with the
VLA at 1.4 GHz (1.7'' FWHM - Morrison et al. 2010; Biggs & Ivison 2006)
and Spitzer at 24, 70 and 160
m; we make use of these
data, as well as the 850-, 1100- and 1250-
m images of
Borys et al. (2003), Perera et al. (2008) and Greve et al. (2008).
We employ three GOODS-N galaxy samples, all selected above a signal-to-noise
threshold of 5:
- 1.
- 128 galaxies selected at 250
m, without priors, with
mJy (Fig. 1; Smith et al., in prep.);
- 2.
- 247 galaxies selected at 1.4 GHz (Fig. 1)
with a 1.4 limit of
20
Jy, 137 with spectroscopic redshifts (Barger et al. 2008), the remainder with photometric redshifts (
; interquartile z, 0.56-1.76);
- 3.
- a
-matched sample of 652 sources spanning z=0-2, selected initially at 24
m (Magnelli et al. 2009; Berta et al. 2010) then filtered to cover only the decade of
between 10
(LIRGs), where
is determined using the models of Chary & Elbaz (2001).
![]() |
Figure 1:
250- |
Open with DEXTER |
Far-IR and submm flux densities for the three samples are determined
using images convolved with appropriate point spread functions.
is calculated by integrating under the well-sampled SEDs. Monte-Carlo
simulations are used to assess the uncertainty in
.
The formal
error on
was boosted by 3
to account for the
uncertain shape of the SED between rest-frame 8-70
m. A
modified blackbody fit to the measurements beyond 24
m (with the
emissivity index,
)
was used to determine
.
For sample (1), additional procedures are implemented to define a
clean sample, free from blends: following the procedure of
Downes et al. (1986), 107/128 sources are found to have secure (P<0.05)
radio identifications (ids) within a search radius, r=10''; we
discard the remainder. To avoid using those sources most severely
affected by blending, we further discard those with more than one
radio emitter within r, leaving 65 sources. Of the galaxies without
a secure radio id, three have no plausible radio ids within r: a
potentially interesting sub-sample. Measurements are made at the
radio positions for the 65 sources with secure, unambiguous ids, and
at the 250-m positions for the three sources without radio
emission.
For sample (2), far-IR and submm measurements are made at the radio positions.
For the
-matched galaxies (sample 3), median stacking is used to
measure
and 1.4: we follow the procedure outlined by
Ivison et al. (2010). Fluxes are calculated from 312-pixel2 stacked
images in the ten available filters and
is determined as before.
3 Results and conclusions
![]() |
Figure 2:
|
Open with DEXTER |
![]() |
Figure 3:
|
Open with DEXTER |
as utilised here is the logarithmic ratio of the rest-frame
8-1000-
m flux,
,
and the 1.4-GHz flux density,
,
such that
= log10 [(
/
W m-2)/ (
/W m-2 Hz-1)], where
is k-corrected assuming
,
with
.
We begin with sample (1), those selected at 250 m:
is
not a strong function of
(Fig. 2), nor of 1.4. We see
no evidence of contamination by radio-loud AGN, consistent with the
findings of Yun et al. (2001). Some galaxies stand out as potentially
far-IR-bright: these include the three galaxies without plausible
radio ids, two of which are detected at 70 and/or 160
m, so are
likely at low redshift with their radio emission resolved away.
Only 39/65 sources with unambiguous radio ids have redshifts (20
photometric, 19 spectroscopic;
;
interquartile z = 0.46-1.52, similar to sample 2). Nevertheless,
this sub-sample allows us to explore correlations between
and
luminosity, redshift and
.
We find significant (>95% confidence
- Table 1) trends for lower
amongst the most radio-
and far-IR-luminous galaxies, and the warmest and most distant, though
these parameters are likely inter-related. The dependence of
on
1.4 is the strongest and likely reflects the influence of
low-radio-power AGN, of which more later; that of
on
is
more puzzling, perhaps reflecting the dependence of
on redshift
and/or
(e.g. Chapman et al. 2005), or selection effects (since
this trend is not seen for sample 2 - see Table 1).
Table 1: Trends.
Figure 3 shows
versus redshift for our radio-selected
galaxies (sample 2), split into five log-spaced bins of
1.4. Does
evolve with redshift? One might conclude that it does, based on
the bottom panel of Fig. 3, where
,
with
(Table 1). However, we must be aware of some strong
selection effects which make this evidence unreliable: radio emission
can be due to an AGN and several radio-loud objects with low values of
are obvious in Fig. 3. Such AGN are more common at
than today (e.g. Wall et al. 2005); moreover, radio emission
from faint starbursts (with
,
although see
Ibar et al. 2010) becomes more difficult to detect at higher
redshifts, such that the fraction of radio-loud AGN in a flux-limited
sample will rise, driving down
.
Indeed, Fig. 4 shows
tentative evidence of a break in
at
1.4
W Hz-1. One might also
expect radio-loud objects (those with low
)
to contain warmer,
AGN-heated dust, giving rise to the weak trend (89.2% confidence -
Table 1) of decreasing
with increasing
.
![]() |
Figure 4:
Median
|
Open with DEXTER |
![]() |
Figure 5:
|
Open with DEXTER |
Finally, we turn to our
-matched galaxies (sample 3), illustrated
in Fig. 5. The
bins provide significant
numbers of objects at near-constant
spanning z=0-2. As well as
being matched in
,
there is another key difference between our new
sample and that used by Ivison et al. (2010): although the new sample is
based initially on a flux-limited 24-
m catalogue, the final
selection is based on
,
with model-dependent extrapolations from
the mid-IR (accurate to
across all bins -
Fig. 5). This should lead to less contamination by AGN at the
blue end of the rest-frame 8-1000-
m band, where the relative
contribution to
can be substantial (Fig. 11
- Ivison et al. 2010). Using our new sample, there is no strong evidence
that
changes as we move back into the epoch of galaxy formation
at
,
with
where
,
consistent with the findings of Sargent et al. (2010b).
If we discount the z<0.5 data, which comprise only 16 galaxies which
are not well matched in
to the higher redshift bins, we find
.
This is similar to the
found by Ivison et al. (2010) who noted reports that evolution in
could be related to the radio background seen by ARCADE 2
(Seiffert et al. 2010; Fixsen et al. 2009). Our sample, with
Jy at
,
is consistent with
the idea that evolution of the FIRRC might be driven by <10-
Jy
radio activity amongst ordinary star-forming galaxies at z>1(Singal et al. 2010).
The data presented in this paper will be released through the Herschel Database in Marseille HeDaM ( hedam.oamp.fr/HerMES). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICYT/MCYT (Spain).
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Footnotes
- ...Herschel
- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
- ... HerMES
- hermes.sussex.ac.uk
All Tables
Table 1: Trends.
All Figures
![]() |
Figure 1:
250- |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
|
Open with DEXTER | |
In the text |
![]() |
Figure 3:
|
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Median
|
Open with DEXTER | |
In the text |
![]() |
Figure 5:
|
Open with DEXTER | |
In the text |
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