A&A 372, L45-L49 (2001)
DOI: 10.1051/0004-6361:20010579
M. Pierre1 - C. Lidman2 - R. Hunstead3 - D. Alloin2 - M. Casali4 - C.
Cesarsky2 - P. Chanial1 - P.-A. Duc1 -
D. Fadda1 - H. Flores1 - S.
Madden1 - L. Vigroux1
1 - CEA Saclay, DSM/DAPNIA, Service d'Astrophysique,
91191 Gif-sur-Yvette, France
2 - European Southern Observatory,
Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
3 - School of Physics, University of Sydney, NSW 2006,
Australia
4 - Royal Observatory, Blackford Hill, Edinburgh EH9
3HJ, UK
Received 31 January 2001 / Accepted 23 April 2001
Abstract
We report the discovery of an extremely red object (ERO) in a
medium-deep ISOCAM extragalactic survey. The object is also a radio
source. Subsequent VLT NIR spectroscopy revealed a prominent Hline giving a redshift of 1.5. We present the spectrum and photometric
data points and discuss evidence that ISO J1324-2016 is a quasar harbouring a
significant amount of very hot dust.
Key words: infrared: galaxies - quasars: general - galaxies: starburst - quasar: individual: ISO J1324-2016
In the course of the ISOCAM Core Programme devoted to the observation
of
galaxy clusters (DEEPXSRC), we have discovered a faint
field source at 7.5 and 15
m with no obvious counterpart on
medium deep optical images. This object was thus a potential
"extremely red object" (ERO), but for the first time, being
directly unveiled through mid-infrared (MIR) observations. The new ERO
class, usually defined by R-K > 5 or R-K > 6, is not only rapidly
growing in size but also in astrophysical relevance. Indeed, it may
shed light on the still hotly debated question of AGN/starburst
connections, the formation epoch of ellipticals as well as the
existence of dust within the crucial redshift range 1 < z < 3. For
an up-to-date review on the ERO topic, see for instance Liu et al.
(2000). Here, we describe the follow-up observations we have
undertaken in order to determine the redshift and to shed light on the
nature of this peculiar object. The next section presents the
spectroscopic and photometric data from X-ray to radio
wavelengths. Section 3 discusses possible interpretations in
conjunction with information provided by galaxies and other EROs at
comparable redshift. Throughout the paper, we assume
H0 = 75 kms-1Mpc-1and q0 = 0.
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Figure 1: Finding charts for ISO J1324-2016. The images are 45'' on a side; North is up, East is left. Left: ESO NTT/SUSI I image (exp. time: 1800 s). Right: ESO VLT/ISAAC K acquisition image (exp. time: 40 s). |
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Figure 2:
Right: portion of the ISAAC H-band spectral interval
showing the H![]() ![]() ![]() |
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Observed | Rest | Flux | Telescope/ |
Wavelength | Wavelength | Density | Instrument |
![]() ![]() |
0.176 ![]() |
<0.98 ![]() |
CFHT (1993) |
![]() ![]() |
0.28 ![]() |
<2.8 ![]() |
CFHT (1993) |
![]() ![]() |
0.36 ![]() |
3.0 ![]() ![]() |
NTT/SUSI (1997) |
![]() ![]() |
0.88 ![]() |
67 ![]() ![]() |
UKIRT (1998) & VLT/ISAAC (2000) |
LW2 6.75 [5-8.5] ![]() |
2.7 ![]() |
0.89 -0.33+0.47 mJy | ISOCAM (1996) |
LW3 15 [12-18] ![]() |
6.0 ![]() |
0.76 -0.40+0.87 mJy | ISOCAM (1996) |
13 cm | 5.0 cm | 0.8 ![]() |
ATCA (1995) |
22 cm | 8.9 cm | 1.4 ![]() |
ATCA (1995) |
35 cm | 14.2 cm | <2.1 mJy | MOST (1993) |
Radio data
The cluster A1732 was observed with the
Australia Telescope Compact Array (ATCA) on 1995 April 18 at
frequencies of 1.344 and 2.378 GHz. Total integration time was 10 hours
in the 6C array, which gives interferometer spacings from
153 m-6 km. The synthesised half-power beamwidths at the declination
of A1732 were
(PA
)
at 1.344 GHz
and
(PA
)
at 2.378 GHz. The
primary flux density calibrator was PKS B1934-638, with B1245-197
and B1622-297 as secondary phase calibrators. ISO J1324-2016 appeared as an
unresolved radio source, with a fitted position of
,
(J2000), and flux densities of
and
mJy at 1.344 and 2.378 GHz,
respectively. The spectral index over this interval is
(
). The 0.5'' radio positional
accuracy was essential for the follow-up identification work.
Optical/NIR broad-band imaging
From 1993 CFHT images of A1732,
the following upper limits on ISO J1324-2016 were set: B> 24.5, R >
22.7. However, since the source was close to the CCD edge, and
affected by vignetting, these limits do not provide a useful
constraint. The source was then observed in 1997 (March 05-06) at ESO
with NTT/SUSI for two hours in the I band; the seeing was
0.6''. In the radio error box, we discovered an object with
(see Fig. 1). The I image of the identification is
unambiguously pointlike (
FWHM < 0.6''). Subsequently, we obtained a
UKIRT service image (1998 April 21) of the field and measured a Kmagnitude of 17.5. This magnitude of
was later
confirmed by the VLT/ISAAC acquisition image (see Fig. 1); moreover,
with a seeing of 0.4'', the ISAAC K image of ISO J1324-2016 remains
pointlike. The I-K color of 4.9 emphasises the extreme redness of
the source spectrum - at least in the observed frame - and the
present lower limit, R-K > 5.2, reinforces the status of ISO J1324-2016 as an
ERO.
X-ray observations
The field of Abell 1732 was observed
with the ROSAT HRI for 30 ks (1996 January 15-27; Pierre
et al. 1996) and with ASCA for a total integration time of
90 ks
and
100 ks by the SIS and GIS instruments
respectively (1997 July 6-7; Pierre et al. 1999). ISO J1324-2016 is not
detected by the HRI. This sets a 3
flux upper limit of
erg s-1 cm-2 in the [0.1-2.4] keV
band, assuming a standard power-law spectrum with a photon index
of 2 (or
erg s-1 cm-2 if corrected
for Galactic absorption). In the [0.4-10] keV ASCA images,
because of the large instrumental point spread function, the
cluster image encompasses the ISO J1324-2016 position, making its detection
impossible.
The NIR spectroscopy
A 2-hour spectroscopic observation
(1998 May 23) at intermediate resolution with EFOSC on the ESO 3.6-m
telescope over the range 4000-9000 Å did not reveal any
significant absorption/emission features.
This stressed the need for deep NIR spectroscopy with a larger
telescope. ISO J1324-2016 was observed with the low resolution spectroscopic
mode of VLT1/ISAAC on 2000 June 7 & 9. Three grating settings
were used to cover the 1.1-2.5 m range. As is standard in
the IR, the target was observed at two positions along the slit
(which we shall call the A and B beams). The bright and variable
night sky lines were removed by subtracting the respective spectra
from each other. The resulting two-dimensional spectra were then
corrected for slit distortion and wavelength calibrated with the
OH lines or with arc lamps.
Residual lines from the night sky were then removed by combining
spectra from the A and B beams. This process works well enough that
one-dimensional spectra can be extracted without any need for
additional sky subtraction. In addition to ISO J1324-2016, two hot stars, with
spectral type A0 or earlier, were observed with the same instrument
configuration. These stars were used to remove telluric features in
the spectra of ISO J1324-2016.
The one-dimensional spectra are shown in Fig. 2; spectral resolution
is 21.4 and 28.4 Å in the J and H bands respectively. The
redshift from the H
line is
.
The H
and [OIII] lines show a relative blueshift of some 1500 and 800
km s-1 respectively. The Balmer decrement is uncertain
because the H
line is very noisy (due to a sky line at 1.215
m) and appears to be narrower than H
;
the estimated value of
20+10-4 is significantly higher than more common values of
5-10. The total corresponding B extinction would be
AB =
7+2-1 in the source restframe, assuming standard extinction
laws (Mathis 1990).
We note first that, although ISO J1324-2016 is in the field of A1732, it is
certainly not a lensed object (at least in the strong regime), since
it is located 0.8 Mpc (4.8') in projected distance from the cluster
centre. The VLT/ISAAC spectrum unambiguously demonstrates that ISO J1324-2016 is
powered by an active nucleus, a fact already suggested by its
pointlike appearance in the I and K bands, together with its radio
activity. The H
FWHM (
3000 km s-1) and rest frame
equivalent width (300 Å) are very similar to those seen in other
high redshift quasars (Espey et al. 1989).
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Figure 3:
Rest frame spectral energy distribution (SED) of ISO J1324-2016 (filled circles) compared with typical local galaxy SEDs from Schmitt
et al. (1997). The template spectra have been normalised to the Kmagnitude point. The dashed line is the averaged SED and the dotted
line gives the observed 1![]() |
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Figure 4:
Rest frame SED of ISO J1324-2016 (filled circles) compared with the
strong starburst HR10 (open circles), an ERO with a similar
redshift. The HR10 spectrum (Elbaz et al. 2001) has been normalised
by a factor 2.4 in order to match the observed K magnitude of
ISO J1324-2016. The line shows the best fit to the HR10 points assuming a pure
starburst model, constrained particularly in the MIR range by the
ISOCAM CVF dataset on local galaxies (Chanial 2001). No LW2 (5-8.5 ![]() ![]() ![]() |
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In conclusion, ISO's MIR view, combined with radio imaging and NIR
spectroscopy, has proven to be an efficient way of identifying a
dusty quasar at z = 1.5. Recent ISOPHOT results on PG quasars
have already revealed considerable dust emission between 25-200 m
(Haas et al. 2000). In ISO J1324-2016 ISOCAM provides evidence for
the presence of hot dust (at 2.7
m, rest frame) heated by an
active nucleus. In this respect, ISO J1324-2016 appears to be a rare object.
With the present data it is not possible to gauge the magnitude of
a possible starburst contribution to the observed MIR
luminosity. Higher resolution optical, infrared and radio imaging may
enable a morphological study of ISO J1324-2016, which may in turn shed light on
the origin of the active nucleus; so far, only 10% of the ERO
population remain unresolved by HST (Stiavelli
2000). FIR/submillimeter observations would sharpen the SED picture,
revealing the presence of cooler dust - responsible for the large
peak predicted by the model in Fig. 4 - associated with star
formation activity.
Acknowledgements
We are grateful to F. Comeron and J.-G. Cuby for help in preparing and performing the VLT/ISAAC observations presented here.