A&A 372, L45-L49 (2001)
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
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.
|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 line at a redshift of 1.50. The original spectrum has been lightly filtered by a Gaussian with a of 1 pixel (3.6 Å). Intensity is in arbitrary units. Left: portion of the ISAAC J spectral interval containing the H and [OIII] lines. No line is detected in the K-band spectrum. In each panel, the lower curve is the noise spectrum extracted from the same data.|
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|0.44 m||0.176 m||<0.98 Jy||CFHT (1993)|
|0.70 m||0.28 m||<2.8 Jy||CFHT (1993)|
|0.90 m||0.36 m||3.0 Jy||NTT/SUSI (1997)|
|2.2 m||0.88 m||67 Jy||UKIRT (1998) & VLT/ISAAC (2000)|
|LW2 6.75 [5-8.5] m||2.7 m||0.89 -0.33+0.47 mJy||ISOCAM (1996)|
|LW3 15 [12-18] m||6.0 m||0.76 -0.40+0.87 mJy||ISOCAM (1996)|
|13 cm||5.0 cm||0.8 0.10 mJy||ATCA (1995)|
|22 cm||8.9 cm||1.4 0.12 mJy||ATCA (1995)|
|35 cm||14.2 cm||<2.1 mJy||MOST (1993)|
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.
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 Hand [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).
|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 dispersion. Open circles are upper limits. The average SED of spirals appears to be quite similar to that of ellipticals and thus is not presented here. The radio data do not constrain the optical-MIR SED but are shown here for completeness.|
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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 m) value is available for HR10; instead, LW10 (8-15 m) was obtained. Note that the well known weak 3.3 m (rest frame) PAH line marginally affects the LW2 band, whereas it is fully encompassed by the LW10 band.|
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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.
We are grateful to F. Comeron and J.-G. Cuby for help in preparing and performing the VLT/ISAAC observations presented here.