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Home All issues Volume 565 (May 2014) A&A, 565 (2014) A19 Full HTML
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Issue
A&A
Volume 565, May 2014
Article Number A19
Number of page(s) 4
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201323004
Published online 25 April 2014

© ESO, 2014

1. Introduction

Following the discovery in large numbers of type 2 quasars (QSO2) in the last decade, an intensive follow up has been performed at different wavelengths: X-ray, radio, infrared, and optical (e.g., Szokoly et al. 2004; Lacy et al. 2007; Martínez-Sansigre et al. 2006; Zakamska et al. 2003). In spite of this, the molecular gas content of this class of objects has been very scarcely studied.

The study of the molecular gas content in these objects is crucial to better understand the conditions required to trigger both the nuclear and star formation activities in the most luminous active galaxies (AGN), since this gaseous phase can provide large amounts of fuel to form stars and feed the nuclear black hole. It can also provide information about the relation between QSO2 and other systems such as type 1 quasars (QSO1), luminous (LIRG, 1011L⊙ ≤ LIR< 1012L⊙) and ultra-luminous (ULIRG, LIR ≥ 1012 L⊙) infrared galaxies, where LIR is the total infrared luminosity (~8–1000 μm range). However, only a few molecular gas studies of QSO2 have been carried out, and frequently focussed on z > 2 objects (see Villar Martín et al. 2013, hereafter VM13, and references therein).

Table 1

The sample.

2. QSO2 sample at z < 1

There are measurements for 29 QSO2 at z< 1 published in three different works. Only 15 CO(1–0) confirmed detections are reported (i.e., 52% detection rate), which imply molecular gas masses M(H in the range (0.5–15) × 109M⊙1.

Krips et al. (2012, hereafter KNC12) investigated the molecular gas content of ten QSO2 at z ~ 0.1–0.4 based on observations performed with the Plateau de Bure Interferometer (PdBI) of the Institut de Radio Astronomie Millimétrique (IRAM). All but two objects (selected from Zakamska et al. 2003), are from the original sample of 24 μm selected galaxies observed with the Spitzer infrared spectrograph for the 5 millijanksy Unbiased Spitzer Extragalactic Survey (5MUSES, Wu et al. 2010, see also Lacy et al. 2007). In KNC12, they confirm the detection of CO(1–0) in five sources and tentative detect a sixth. The molecular gas masses were found in the range of M(H2) ~ (0.4−2.6) × 109 M⊙ for the detections and upper limits are in the range (0.4–2.2) × 109 M⊙ for the non-detections.

In VM13, we presented the results of CO(1–0) spectroscopic observations of ten QSO2 at z ~ 0.2–0.34 performed with the 30 m IRAM radiotelescope and the Australia Telescope Compact Array. All objects were selected from the original sample of QSO2 at 0.3 ≲ z ≲ 0.8 identified by Zakamska et al. (2003) from the Sloan Digital Sky Survey (SDSS, York et al. 2000). Five new confirmed CO(1–0) detections were reported, with M(H2) ~ (5–6) × 109M⊙, and one tentative detection. Upper limits are in the range (1.6–5.0) × 109M ⊙ for the non-detections.

Most of these 20 QSO2 (17/20) have LIR< 1012L⊙, i.e., in the LIRG regime or below. Only three have LIR ~ 1012L⊙ in the transition between the LIRG and ULIRG regimes. The implied molecular gas masses are found to be consistent with QSO1 of similar infrared luminosities.

Here we expand our work into the ULIRG regime. We include results of CO(1–0) observations of four ULIRG SDSS QSO2 at z ~ 0.3 (Table 1), to match in z the sample by VM13.

We also include nine objects in the z ≲ 1 ULIRG samples by Combes et al. (2011, 2013; C11 and C13 hereafter). Making use of either the original SDSS spectra when available or optical line luminosities published in the literature, we find that the following ULIRG can be classified as QSO2 according to Zakamska et al. (2003) criteria: G19, G30, S1, S4, S8, S10, S12, S21, S25 (the nomenclature in C11, C13 is used). These nine QSO2 are at z ~ 0.3–0.9. Spectroscopic observations of different CO transitions performed with the IRAM 30 m radiotelescope imply M(H2) ~ (3.2–15.4) × 109 M⊙ for the five detections and upper limits ~(1.1–7.2) × 109 M⊙ for the four non-detections (C11, C13).

thumbnail Fig. 1

CO(1–0) spectra of the four QSO2 in our sample. The zero velocity corresponds to zSDSS. A fit of the line profile is shown in green for the object with detected emission. The vertical axis shows the corrected-beam temperature. The bottom box represents the velocity window where the line is expected.

We assume ΩΛ = 0.7, ΩM = 0.3, H0 = 71 km s-1 Mpc-1.

3. Observations and data reduction

Table 2

Luminosity (2) of the [OIII]λ5007 line (Zakamska et al. 2003) is given in logarithmic units of L⊙.

thumbnail Fig. 2

vs. z (top) and vs. LFIR (bottom) for QSO1 (blue symbols) and QSO2 (green symbols). Our four ULIRG QSO2 are the red open circles. References are as follows: green solid circles: QSO2 from VM13. Open green squares: QSO2 from KNC12. Green solid squares: QSO2 from C11 and C13. Green solid triangles: z ≥ 2 QSO2 from different works (DW) (Aravena et al. 2008; Martínez Sansigre et al. 2009; Yan et al. 2010; Polleta et al. 2011; Lacy et al. 2011) // Blue crosses: z ≥ 2 QSO1 from different works (DW) (Cox et al. 2002; Carilli et al. 2002; Walter et al. 2004; Krips et al. 2005; Riechers et al. 2006, 2009a,b; Gao et al. 2007; Maiolino et al. 2007; Coppin et al. 2008; Wang et al. 2010, 2011). Blue solid squares: QSO1 from C11 and C13. Open blue circles: z ≤ 0.2 QSO1 from different works (DW) (Evans et al. 2001, 2006; Scoville et al. 2003; Pott et al. 2006; Bertram et al. 2007). Filled blue circles: ULIRG QSO1 from Xia et al. 2012 (X12). Orange small diamonds: star forming ULIRGs at z ≤ 1 (C11, C13; Graciá Carpio et al. 2008 (GC08))

The observations were carried out using the 30 m IRAM single dish telescope at Pico Veleta, during two different observing runs in February and June 2013 (programme 202-12). The EMIR receiver was tuned to the redshifted frequencies of the CO(1–0) line (115.27 GHz rest frame), using the optical SDSS z for each object (see Table 1). The observations were performed in the wobbler-switching mode with a throw 50′′ to ensure flat baselines. We observe both polarizations (H and V) using as a backend the WILMA autocorrelator that produced an effective total bandwidth of 4 GHz with a (Hanning-smoothed) velocity resolution of 16 MHz ~ 50 km s-1. The corresponding Tsys, total integration time and the rms corresponding for each source is specified in Table 1. The temperature scale used is in main beam temperature Tmb. At 3mm the telescope half-power beam width is 29″. The main-beam efficiency is and the conversion factor is Jy/K.

The pointing model was checked against bright, nearby calibrators for every source, and every 1.6 h for long integrations. It was found to be accurate within 5″. Calibration scans on the standard two load system were taken every 8 min.

The off-line data reduction was done with the CLASS programme of the GILDAS software package (Guilloteau & Forveille 1989), and involved only the subtraction of (flat) baselines from individual integrations and the averaging of the total spectra (Fig. 1).

4. Results

4.1. Infrared luminosities

The four QSO2 in our sample have an IRAS counterpart at 60 and/or 100 μm, wich we have used to constrain the far-infrared luminosities LFIR. For coherence with numerous works published in the literature, we estimate LFIR in the 40–500 μm range applying FFIR = 1.26 × 10-11 [2.58 f60 + f100] erg s-1 cm-2 and , where we assume C = 1.42 (Mirabel & Sanders 1996). The IRAS flux densities are f60 and f100 at 60 and 100 μm in Jy. Although the formula was derived for star forming galaxies at z = 0, it is also often used for AGN and galaxies at higher z. Thus, here we consider it adequate for the purpose of comparison with other works (e.g., C11, C13, Bertram et al. 2007).

Measurements in both the 60 and 100 μm bands exist only for SDSS J0903+02, while IRAS detections are reported only in one of the bands for the other three QSO2. In such cases, we have constrained the flux in the missing band by assuming typical values of Q = f60 μm/f100 μm for similar objects. There are 12 SDSS QSO2 at z ~ 0.3–0.4 with IRAS measurements in both bands (Zakamska et al. 2004). These show Q median, average and standard deviation values 0.26, 0.29 and 0.17, respectively. Approximately, 10/12 (83%) of these QSO2 have Q in the range 0.29 ± 0.15. The most probable LFIR values and their uncertainties for SDSS J1337-01, SDSS J1520-01 and SDSS J1543-00 have been calculated by using Q = 0.29 ± 0.15. Following VM13, LIR was then constrained by assuming a typical .5. The results are shown in Table 2. The errors reflect the uncertainty on the range of possible Q values. The four QSO2 have LIR in the ULIRG regime (>1012L⊙).

4.2. Calculation of L and M(H2)

Detection of CO(1–0) is confirmed in one object (SDSS J1543-00) with  ± 0.2)× 1010 K km s-1 pc2 (Table 2). Optical images of this quasar show that it is undergoing a major merger event (Villar Martín et al. 2012). Assuming α = 0.8 M⊙ (K km s-1 pc2)-1, the implied molecular gas mass is (9.6 ± 1.6) × 109M⊙, which is consistent with molecular gas content of other systems with similar LIR. A 1-Gaussian fit of the line profile implies FWHMCO = 576 ± 102 km s-1 with a velocity redshift relative [OIII]λ5007 of 128 ± 47 km s-1. No CO(1–0) is detected in the other three QSO2. Following the same procedure described in VM13, 3σ upper limits on the molecular gas masses are estimated to be 9.6, 4.3, and 5.4 × 109 M⊙ for SDSS J0903+02, SDSS J1337-01, SDSS J1520-01, respectively.

The location of the four objects in the vs. z and vs. LFIR and diagrams is shown in Fig. 2 as red hollow circles (see VM13 for a detailed discussion), with other QSO1 (blue symbols) and QSO2 (green symbols) samples (left panels) and star forming ULIRGs at ≲1 (right panel). The nine ULIRG QSO2 from C11 and C13 are represented with green solid squares. These 13 ULIRG QSO2 at z< 1 fall on the vs. LFIR correlation defined by other quasar samples at different z and overlap with the location of star forming ULIRG. The LFIR is likely to be dominated by the starburst contribution in those QSO2 with total LIR< 2 × 1012L⊙. This is less certain at higher luminosities, where an increasing relative contribution of the AGN might occur (Nardini et al. 2010). Indeed, several QSO2 and QSO1 from Combes et al. (2011, 2013) are at the lower envelope of the data distribution in the vs. LFIR diagram. This might suggest a poor gas content compared with star forming ULIRGs of similar LFIR. It is, possible however, that this effect is a consequence of a substantial contribution of the AGN to the LFIR, since all of them have LIR> 2 × 1012L⊙, above the turning point identified by Nardini et al. (2010).

5. Conclusions

We present the results of CO(1–0) spectroscopic observations of four SDSS QSO2 at z~ 0.3 observed with the 30 m IRAM telescope. These QSO2 have infrared luminosities in the ULIRG regime, expanding our previous work on less infrared luminous QSO2 at z ~ 0.3 into this regime. The four QSO2 have LFIR ~ (1–2.5) × 1012L⊙. We have also added nine ULIRG QSO2 at z ~ 0.3–0.9 from Combes et al. (2011, 2013), which have LFIR ~ (0.2–2.5) × 1013L⊙.

Detection of CO(1–0) is confirmed in one of the four objects observed by us: SDSS J1543-01. and MH2 are (1.2 ± 0.2) × 109 K km s-1 pc2 and (9.6 ± 1.6) × 109M⊙, respectively. The line has FWHM = 575 ± 102 km -1. No CO(1–0)

emission is detected in SDSS J0903+02, SDSS J1337-01, SDSS J1520-01. The 3σ upper limits on M(H2) are 9.6, 4.3 and 5.4 × 109M⊙, respectively.

The (measurements and upper limits) of all 13 ULIRG QSO2 at z< 1 fall in the vs. LFIR and vs. z correlations defined by QSO1 and QSO2 with different z and LIR. They overlap well as with z< 1 star forming ULIRGs. Several QSO1 and QSO2 in Combes et al. (2011, 2013) mark the lower envelope defined by the scatter of the correlation. They might be gas poor objects. Alternatively, this result might be an effect of a significant contribution of the AGN to the LFIR.

1

For coherence with other works, we assume α = 0.8 M⊙ (K km s-1 pc2)-1 (Downes & Solomon 1998). Recent results suggest α = 0.6 ± 0.2 (Papadopoulos et al. 2012).

Acknowledgments

M.R. acknowledge support by the Spanish MINECO through grant AYA 2012-38491-C02-02, cofunded with FEDER funds. This work has been funded with support from the Spanish former Ministerio de Ciencia e Innovación through the grant AYA2010-15081. Thanks to the staff at IRAM Pico Veleta for their support during the observations. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).

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All Tables

Table 1

The sample.

In the text
Table 2

Luminosity (2) of the [OIII]λ5007 line (Zakamska et al. 2003) is given in logarithmic units of L⊙.

In the text

All Figures

thumbnail Fig. 1

CO(1–0) spectra of the four QSO2 in our sample. The zero velocity corresponds to zSDSS. A fit of the line profile is shown in green for the object with detected emission. The vertical axis shows the corrected-beam temperature. The bottom box represents the velocity window where the line is expected.
In the text
thumbnail Fig. 2

vs. z (top) and vs. LFIR (bottom) for QSO1 (blue symbols) and QSO2 (green symbols). Our four ULIRG QSO2 are the red open circles. References are as follows: green solid circles: QSO2 from VM13. Open green squares: QSO2 from KNC12. Green solid squares: QSO2 from C11 and C13. Green solid triangles: z ≥ 2 QSO2 from different works (DW) (Aravena et al. 2008; Martínez Sansigre et al. 2009; Yan et al. 2010; Polleta et al. 2011; Lacy et al. 2011) // Blue crosses: z ≥ 2 QSO1 from different works (DW) (Cox et al. 2002; Carilli et al. 2002; Walter et al. 2004; Krips et al. 2005; Riechers et al. 2006, 2009a,b; Gao et al. 2007; Maiolino et al. 2007; Coppin et al. 2008; Wang et al. 2010, 2011). Blue solid squares: QSO1 from C11 and C13. Open blue circles: z ≤ 0.2 QSO1 from different works (DW) (Evans et al. 2001, 2006; Scoville et al. 2003; Pott et al. 2006; Bertram et al. 2007). Filled blue circles: ULIRG QSO1 from Xia et al. 2012 (X12). Orange small diamonds: star forming ULIRGs at z ≤ 1 (C11, C13; Graciá Carpio et al. 2008 (GC08))
In the text

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