Issue |
A&A
Volume 518, July-August 2010
Herschel: the first science highlights
|
|
---|---|---|
Article Number | L15 | |
Number of page(s) | 5 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361/201014593 | |
Published online | 16 July 2010 |
Herschel: the first science highlights
LETTER TO THE EDITOR
Improving the identification of high-z
Herschel sources with
position priors and optical/NIR and FIR/mm photometric redshifts![[*]](/icons/foot_motif.png)
P. G. Pérez-González1,2 - E. Egami2 - M. Rex2 - T. D. Rawle2 - J.-P. Kneib3 - J. Richard4 - D. Johansson5 - B. Altieri6 - A. W. Blain7 - J. J. Bock7,8 - F. Boone9 - C. R. Bridge7 - S. M. Chung10 - B. Clément3 - D. Clowe11 - F. Combes12 - J.-G. Cuby13 - M. Dessauges-Zavadsky14 - C. D. Dowell7,8 - N. Espino-Briones1 - D. Fadda15 - A. K. Fiedler2 - A. Gonzalez10 - C. Horellou5 - O. Ilbert3 - R. J. Ivison16,17 - M. Jauzac3 - D. Lutz18 - R. Pelló9 - M. J. Pereira2 - G. H. Rieke2 - G. Rodighiero19 - D. Schaerer14 - G. P. Smith20 - I. Valtchanov6 - G. L. Walth2 - P. van der Werf21 - M. W. Werner8 - M. Zemcov7,8
1 - Departamento de Astrofísica, Facultad de CC. Físicas, Universidad
Complutense de Madrid, 28040 Madrid, Spain
2 - Steward Observatory, The University of Arizona, 933 N Cherry
Avenue, Tucson, AZ 85721, USA
3 - Laboratoire d'Astrophysique de Marseille, CNRS - Université
Aix-Marseille, 38 Rue Frédéric Joliot-Curie, 13388 Marseille, France
4 - Institute for Computational Cosmology, Department of Physics,
Durham University, South Road, Durham DH1 3LE, UK
5 - Onsala Space Observatory, Chalmers University of Technology, 439 92
Onsala, Sweden
6 - Herschel Science Centre, ESAC, ESA, PO Box
50727, 28080 Madrid, Spain
7 - California Institute of Technology, Pasadena, CA 91125, USA
8 - Jet Propulsion Laboratory, Pasadena, CA 91109, USA
9 - Laboratoire d'Astrophysique de Toulouse-Tarbes, Université de
Toulouse, CNRS, 14 Av. Edouard Belin, 31400 Toulouse, France
10 - Department of Astronomy, University of Florida, Gainesville,
FL 32611-2055, USA
11 - Department of Physics & Astronomy, Ohio University,
Clippinger Labs 251B, Athens, OH 45701, USA
12 - Observatoire de Paris, LERMA, 61 Av. de l'Observatoire, 75014
Paris, France
13 - Laboratoire d'Astrophysique de Marseille, Observatoire
Astronomique de Marseille-Provence, 2 Place Le Verrier, 13248
Marseille, France
14 - Geneva Observatory, University of Geneva, 51 Ch. des Maillettes,
1290 Versoix, Switzerland
15 - NASA Herschel Science Center, California
Institute of Technology, MS 100-22, Pasadena, CA 91125, USA
16 - UK Astronomy Technology Centre, Science and Technology Facilities
Council, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
17 - Institute for Astronomy, University of Edinburgh, Blackford Hill,
Edinburgh EH9 3HJ, UK
18 - Max-Planck-Institut für extraterrestrische Physik, Postfach 1312,
85741 Garching, Germany
19 - Department of Astronomy, University of Padova, Vicolo
dell'Osservatorio 3, 35122 Padova, Italy
20 - School of Physics and Astronomy, University of Birmingham,
Edgbaston, Birmingham, B15 2TT, UK
21 - Sterrewacht Leiden, Leiden University, PO Box 9513, 2300 RA
Leiden, The Netherlands
Received 31 March 2010 / Accepted 6 May 2010
Abstract
We present preliminary results about the detection of high redshift
(U)LIRGs in the Bullet cluster field by the PACS and SPIRE instruments
within the Herschel Lensing Survey (HLS)
Program. We describe in detail a photometric procedure designed to
recover robust fluxes and deblend faint Herschel
sources near the confusion noise. The method is based on the use of the
positions of Spitzer/MIPS 24 m sources as
priors. Our catalogs are able to reliably (5
) recover
galaxies with fluxes above 6 and 10 mJy in the
PACS 100 and 160
m channels,
respectively, and 12 to 18 mJy in the SPIRE bands. We
also obtain spectral energy distributions covering the optical through
the far-infrared/millimeter spectral ranges of all the Herschel
detected sources, and analyze them to obtain independent estimations of
the photometric redshift based on either stellar population or dust
emission models. We exemplify the potential of the combined use of Spitzer
position priors plus independent optical and IR photometric redshifts
to robustly assign optical/NIR counterparts to the sources detected by Herschel
and other (sub-)mm instruments.
Key words: infrared: galaxies - submillimeter: galaxies - galaxies: evolution - galaxies: high-redshift - gravitational lensing: strong - galaxies: photometry
1 Introduction
Based on the IRAS, ISO, and Spitzer missions, we
know that luminous infrared galaxies (LIRGs) experienced significant
evolution in the past 8 Gyr, roughly decreasing their typical
infrared luminosity [L(IR)] by an order of
magnitude from
to z=0 (Le Floc'h et al. 2005;
Pérez-González
et al. 2005; Rodighiero et al. 2010;
Flores
et al. 1999; Magnelli et al. 2009;
Chary
& Elbaz 2001). By
,
they dominated the star formation activity of the Universe, being
responsible for more than 50% of the cosmic
SFR density up to at least
,
and playing an important role in the formation of massive galaxies at
,
which exhibit high star formation efficiencies (Damen et al. 2009;
Pérez-González
et al. 2008; Reddy et al. 2008),
strong dust obscured nuclear activity (Donley et al. 2008;
Daddi
et al. 2007), or both. Beyond
,
sub-mm surveys have also detected a population of LIRGs and (mostly)
ULIRGs, identified as very active stages in the formation of massive
galaxies (Chapman
et al. 2005,2003; Pope
et al. 2006; Smail et al. 1997;
Hughes
et al. 1998).
Although very useful for measuring the obscuration of optical
light by interstellar dust (very abundant in the most extreme
starbursts), the analysis of IR data to understand
the formation and evolution of galaxies in the Universe has been
classically hampered mainly by two issues. First,
the sensitivity of IR telescopes has increased
significantly from one mission to the next (and also their angular
resolution, although at a lower rate), but there are still problems
correctly identifying all sources detected in IR surveys, most
noticeably at longer wavelengths where confusion remains severe
(e.g., at 70/160 m in the Spitzer/MIPS surveys
and in the SCUBA or
LABOCA sub-mm data). Moreover, finding counterparts and getting
reliable redshifts from spectroscopy for high redshift (U)LIRGs is
challenging since a good fraction of them are extremely faint at
optical/NIR wavelengths (Frayer et al. 2004;
Wilson
et al. 2008; Ivison et al. 2002).
A second problem for the study of
(U)LIRGs is the availability of only one photometric data point
(MIPS 24
m)
for most of them. The fits to
dust emission models to calculate L(IR),
and from this derive a SFR (Kennicutt
1998), need a considerable extrapolation, and thus the SFR is
subject to significant systematic uncertainties (Barro et al. 2010; Daddi
et al. 2007; Papovich et al. 2006).
In addition, the limited FIR data already
available for galaxies at
indicate that they have different dust properties from those observed
for nearby (U)LIRGs (Chapman et al. 2005;
Rieke
et al. 2009; Rigby et al. 2008;
Papovich
et al. 2007).
The ESA Herschel Space Observatory (Pilbratt et al. 2010)
alleviates these two issues. Thanks to its sensitivity and angular
resolution at 100 < <
500
m,
it enables us to robustly characterize high-z
galaxies. In addition to the populations of
IR galaxies newly discovered by Herschel,
it will supply up to six photometric data points in the IR
range for
galaxies
detected by MIPS at 24
m. These data can be used to constrain the fits
to the dust
emission templates. Even more novel and relevant is the combination of Herschel
observations with the MIPS data (and also IRAC) to diminish the effects
of source confusion in IR surveys. The new
Herschel data indeed allow an easier and more
reliable identification of counterparts from one band to the adjacent
one as we move to shorter wavelengths. In addition,
the Herschel bands
effectively fill the gap between MIPS and (sub-)mm surveys (with
SCUBA2, LABOCA, or AzTEC). By combining all these datasets, we
can now use the several IR photometric data points to estimate
a photometric redshift based on dust emission alone, and compare it
with the estimations based on UV-to-NIR data. This can be regarded as
an extension of the radio-to-IR photo-z method
(Carilli
& Yun 1999; Daddi et al. 2009;
Rengarajan
& Takeuchi 2001; Aretxaga et al. 2003;
Blain
et al. 2003; Dunne et al. 2000),
benefiting from a finer sampling of the emission from dust at different
temperatures. The procedure can be used to improve the
cross-correlation with optical/NIR galaxy samples, or even to obtain
the only redshift measurement possible for very faint (high-z)
IR-bright optically-faint sources. These sources may be numerous in the
Herschel surveys, because of its impressive
sensitivity at wavelengths probing the peak of the dust emission, which
can be brighter than the optical emission by orders of magnitude.
In this letter, we perform a preliminary analysis of the Herschel Lensing Survey (HLS, PI Egami) data taken for the Bullet cluster to show the utility of position priors and photometric redshifts obtained from UV-to-NIR and IR-to-mm data to improve the identification of Herschel and sub-mm sources with those detected at shorter wavelengths. A correct identification of IR sources will be extremely relevant to all Herschel cosmological surveys, but is of critical importance for clusters, because of their crowded nature and the possible presence of high-z lensed and distorted sources with very faint optical counterparts that may even only be detectable in the FIR/mm range.
2 Data and catalogs
The reduction of the Herschel SPIRE (Griffin et al. 2010)
and PACS (Poglitsch et al.
2010) data of the Bullet cluster (
06:58,
-55:57) is described in Egami
et al. (2010) and
Rex et al. (2010),
jointly with optical-to-mm ancillary data used to estimate photometric
redshifts, stellar masses, and SFRs. Here we describe our cataloging
procedure for the five Herschel bands:
PACS 100 and 160
m, and SPIRE 250, 350,
and 500
m.
Given the remarkable depth of the Spitzer
MIPS 24 m
images, PACS catalogs have been compiled with a position prior
technique, involving a list of MIPS sources and a PSF fitting analysis
(see Pérez-González
et al. 2008). To improve the reliability of
the method, we first aligned all Herschel images to
the WCS of the MIPS 24
m map using the wcstools
software
(Mink 1999),
obtaining matching uncertainties smaller than one pixel for each Herschel
band. The MIPS 24
m
catalog in the Bullet cluster field has a 5
detection
level of
=
85
30
Jy
, and a density of
5.3 sources/arcmin2 above that
threshold (7.2 sources/arcmin2 with S[24] > 50
Jy).
The similar PSF sizes of the MIPS 24 m and the
PACS 100
m
bands (
6
and
8
,
respectively) make the identification and extraction of sources
straightforward for this band. In addition, we also considered
that some sources may be too faint for MIPS yet still be detectable by
PACS. To account for this population, we detected sources
directly in the PACS data using Sextractor (Bertin & Arnouts 1996),
obtaining a sample of 43 sources above the 5
level
(
= 5.5
0.7 mJy).
The cross-correlation of this sample with the MIPS catalog (using a
search radius of 3
)
revealed that all but one of the robust PACS detections are detected at
24
m,
and 5 of them had 2 MIPS counterparts within the
search
radius. The only non-detection at 24
m is, in fact, a group
of three very faint 100
m sources within 10
,
which are detected as one single source by Sextractor
in the PACS image,
but are individual sources at 24
m. The 5 multiple detections were
sources for which the slightly higher resolution and greater depth of
MIPS allowed the deblending of close IR emitters. This
cross-correlation also found that the WCS alignment between both images
has an rms smaller than 1
.
For the 160 m
image, it is expected that more 24
m sources are merged to form single sources. For
this reason, before measuring photometry, we removed sources from the
main catalog that could not be separated at the resolution of the PACS
160
m
band, i.e., sources closer than 6
,
which is half of the PSF FWHM, keeping only the brightest source at
24
m
for each group of merged sources. The master catalog combined the MIPS
source list with the direct
detections in the 160
m image above the 5
level (
= 10
1 mJy),
all the latter being actually detected in the MIPS data. Merged sources
account for almost 20% of
the master catalog, with 85% (15%) of this subsample having
2 (3) objects within 6
.
Just considering sources directly detected at 160
m, the
fraction of them presenting multiple identifications in the MIPS
catalog is higher than 40%. The WCS accuracy between the
MIPS and PACS160 images is inferior to 1.5
.
The final purged list of sources was used to fit PSFs at the
given positions using the daophot package in IRAF,
allowing for one pixel centering offsets. The results of this PSF
fitting algorithm are flux densities in a given aperture (we found the
optimum values to be 5
and 7.5
for the PACS green and red
channels, respectively), to which
an aperture correction must be applied. The values we applied are
1.84
0.08 and 1.93
0.08 for 100 and 160
m, respectively. We note that these aperture
corrections are larger than those published by the PACS Team, but we
found that their PSF matched ours (constructed with the same Bullet
cluster data) for large radii, but was brighter for similar and smaller
radii than that selected for the PSF fitting method.
![]() |
Figure 1:
Postage stamps of two high-z sources in the Bullet
cluster field detected by Herschel: the southern
tip of the arc MIPS06:58:31.1-55:56:39.2 ( left),
and the LABOCA source MIPS06:58:45.3-55:58:46.5 (
right). The size
of the images is 2 |
Open with DEXTER |
The SPIRE catalogs were also compiled with a method based on priors and
PSF fitting. The photometry was carried out in circular apertures
(of radii 12
,
18
,
and 22
for 250, 350, and
500
m,
respectively), applying a calibration based on
the beam sizes (assuming they are Gaussians). For the 250
m channel,
we combined the list of sources detected by MIPS at 24
m and the
direct detection in the SPIRE data using Sextractor
and a 5
threshold (
= 12
2 mJy).
Other objects within 9
(half of the PSF FWHM) of a
given candidate source were purged, only
the position of the brightest galaxy at 24
m being
kept. For the region covered simultaneously by MIPS and the
SPIRE 250
m
channel, only 2 SPIRE sources out of 261 were not
detected by MIPS, but both of them turned to be F(24)
60
Jy
detections at the 3
level.
Around half of the SPIRE sources have 2 or more MIPS
counterparts within 9
.
The WCS alignment between the MIPS and
SPIRE250 images has an rms of
4
.
Table 1: Properties of the HLS Bullet cluster catalogs.
The catalog for the SPIRE 350 m channel was constructed from the list of
detections at 250
m.
Sources within 14
were merged into the same
object (about 40% of the total
catalog, virtually all of them being a doublet), only the position of
the brightest one at 250
m being kept. A direct detection in the
350
m
image (
= 17
3 mJy)
found that 5% of sources are not directly linked to a
250
m
emitter, but virtually all of these are
a combination of several 250
m sources that causes a displaced 350
m centroid.
Only one isolated high-confidence 350
m source was not detected in the 250
m catalog,
but a reliable flux could be recovered in the blue channel once the
350
m
detection revealed its position. The WCS alignment between the
MIPS and SPIRE350 images has an rms of
6
.
For the 500 m
channel (
= 18
4 mJy), we started from the 350
m catalog, and we did not find any object without
an identification in the bluer bands using a 18
search radius (approximately
half of the PSF FWHM). Around 50%
of the SPIRE 500
m
sources were doublets in the 350
m band. The WCS alignment between the
MIPS and SPIRE500 images has an rms of
9
.
The prior-based photometric technique was compared with the
direct blind detection in the Herschel images.
In PACS, a direct detection down to 5
included more than 40% of sources with no
counterpart in the MIPS map, implying that these are probably spurious
detections. The fluxes of sources extracted with both the blind and
prior-based detections are virtually identical. In SPIRE,
the prior-based procedure is able to recover fluxes for 30%
more sources than the direct detection. For the sources in
common, the average difference in the photometry is 2%
(the blind method provides brighter fluxes), with
a 6% scatter.
Table 1
indicates the surveyed areas, detection thresholds,
the corresponding source densities, and fraction of merged
sources for our catalogs of the PACS and SPIRE HLS data.
An important (and potentially dangerous) step in our
photometric procedure based on position priors is the blending of
nearby non-resolved sources, which provides only the position of the
brightest galaxy in the parent catalog to the PSF fitting algorithm. We
note that the MIPS 24 m flux is dominated by the emission of warm dust
and/or PAHs while the SPIRE bands are dominated by the emission of cold
dust. Thus, it is probable that bright MIR emitters are not
the dominant sources at FIR wavelengths
(see Fig. 1).
In the following section, we illustrate a method to help in
the robust identification and/or deblending of the Herschel
sources.
3 Identification of high-z Herschel sources
Figure 1
shows thumbnails in several bands of two interesting sources detected
by Herschel in the Bullet cluster field:
the southern tip of the arc at z=3.24
described in
Mehlert et al.
(2001), and a sub-mm galaxy detected by LABOCA
(source #10 in Johansson
et al. 2010). With these two examples, we
demonstrate that the use of IRAC and MIPS data helps to correctly
identify the Herschel sources with optical/NIR
counterparts. In the case of the arc, the photometric method based on
the use of the MIPS 24 m catalog as a prior helped in the detection and
measurement processes for the PACS 160
m and SPIRE bands, where the source is very faint
and almost indistinguishable from the background. In the PACS red band,
our method allows a deblending of the source in the two knots detected
by MIPS and linked to the arc. In the case of the LABOCA source,
although it is barely detected in the optical, the position of the
source can be followed as we move to redder wavelengths and larger
PSFs, allowing a more reliable identification in spite of the presence
of a close neighbor to the west. The brightest source at 24
m is indeed
already brighter than its companion at IRAC wavelengths (most
noticeably, at 8.0
m), and this nearby source disappears in PACS.
This illustrates the benefits of the use of Spitzer
data as priors to obtain the most probable identifications of Herschel
and (sub-)mm emitters at shorter wavelengths.
![]() |
Figure 2:
SEDs of the z = 3.24 LIRG
MIPS06:58:31.1-55:56:39.2 (magnification factor |
Open with DEXTER |
Figure 2
shows the optical-to-mm SEDs of the two examples of high-z
galaxies. Photometric redshifts for all 24 m sources in
the Bullet cluster field were estimated from the UV-to-MIR data
(including IRAC fluxes) using the technique described in Pérez-González
et al. (2005,2008). Briefly, the
SEDs compiled from aperture-matched photometry are fitted with stellar
population models and AGN templates from Polletta et al. (2007).
A minimization algorithm is used to search for the optimal
redshifted template fitting the data, and the most probable photometric
redshift is calculated by integrating the redshift probability function
(see
also Barro et al. 2010).
Photometric redshifts were also estimated from the IR data
alone by comparing the Spitzer, Herschel
and (sub-)mm fluxes with dust emission templates from
Chary & Elbaz (2001),
Dale & Helou (2002),
and Rieke et al.
(2009). Using these two fits, we estimated relevant
parameters such as the stellar mass and the SFR. The
Rieke et al. (2009)
template most closely fitting the data for the arc corresponds to a
local L(IR) = 10
galaxy. This value is
consistent with the average for the arc based on
the three template libraries, L(IR) = 10
,
once a magnification factor of
21 is applied (Bradac et al. 2006).
The LABOCA source qualifies as a
hyper-LIRG based on the best fits to all template libraries
(if it is not lensed), and the best-fit template from Rieke
et al. is that of a local galaxy with 10
,
although our source seems to have more prominent PAH emission.
Figure 2
illustrates the power of using independent estimates of the photometric
redshift based on UV-to-NIR data and IR dataalone to validate the
individual values (see the photo-z probability
distributions). The procedure is also useful for achieving more
reliable identifications of the IR emitters.
For example, for the LABOCA source at
,
we calculated photometric redshifts based on UV-to-NIR data for the
three close neighbors detected by MIPS within
10
of the central source. The
galaxy to the north lies at
(a cluster member), that to the south at
,
and the closest companion has a photo-z compatible
with the central source (
0.3),
thus implying that the two sources are a possible
interacting pair.
The general validity of our method for the whole sample of Herschel
sources will be tested thoroughly in forthcoming papers by evaluating
the quality of our photo-z's. From a preliminary
comparison of the optical and FIR photo-z's for
sources detected by MIPS, PACS, SPIRE, and a (sub)-mm
instrument, it is encouraging that we measure an average
=
=
0.09 with 10% of catastrophic outliers (
> 0.2), comparable to
the typical goodness of
IR-based photo-z's (Aretxaga
et al. 2003).
This work is based in part on observations made with Spitzer, operated by JPL/Caltech. We thank the AzTEC Team for letting us use their data. P.G.P.-G. acknowledges support from grants AYA 2006-02358, AYA 2006-15698-C02-02, and CSD2006-00070, and the Ramón y Cajal Program, all financed by the Spanish Government and/or the European Union.
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Footnotes
- ... redshifts
- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
- ...
Jy
- Calculated from several artificial apertures formed with random sky pixels; see Appendix A in Pérez-González et al. (2008).
All Tables
Table 1: Properties of the HLS Bullet cluster catalogs.
All Figures
![]() |
Figure 1:
Postage stamps of two high-z sources in the Bullet
cluster field detected by Herschel: the southern
tip of the arc MIPS06:58:31.1-55:56:39.2 ( left),
and the LABOCA source MIPS06:58:45.3-55:58:46.5 (
right). The size
of the images is 2 |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
SEDs of the z = 3.24 LIRG
MIPS06:58:31.1-55:56:39.2 (magnification factor |
Open with DEXTER | |
In the text |
Copyright ESO 2010
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