Far-infrared properties of submillimeter and optically faint radio galaxiesHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

Far-infrared properties of submillimeter and optically faint radio galaxiesthanks: Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

B. Magnelli (See online Appendix A for author affiliations)    D. Lutz (See online Appendix A for author affiliations)    S. Berta (See online Appendix A for author affiliations)    B. Altieri    P. Andreani    H. Aussel    H. Castañeda    A. Cava    J. Cepa    A. Cimatti    E. Daddi    H. Dannerbauer    H. Dominguez    D. Elbaz    N. Förster Schreiber (See online Appendix A for author affiliations)    R. Genzel (See online Appendix A for author affiliations)    A. Grazian    C. Gruppioni    G. Magdis    R. Maiolino    R. Nordon (See online Appendix A for author affiliations)    I. Pérez Fournon    I. Pérez García    A. Poglitsch (See online Appendix A for author affiliations)    P. Popesso (See online Appendix A for author affiliations)    F. Pozzi    L. Riguccini    G. Rodighiero    A. Saintonge (See online Appendix A for author affiliations)    P. Santini    M. Sanchez-Portal    L. Shao (See online Appendix A for author affiliations)    E. Sturm (See online Appendix A for author affiliations)    L. Tacconi (See online Appendix A for author affiliations)    I. Valtchanov    E.Wieprecht (See online Appendix A for author affiliations)    E. Wiezorrek (See online Appendix A for author affiliations) Magnelli@mpe.mpg.de
Received ??; accepted ??
Key Words.:
Galaxies: evolution - Infrared: galaxies - Galaxies: starburst - Submillimeter: galaxies
offprints: B. Magnelli,

We use deep observations obtained with the Photodetector Array Camera & Spectrometer (PACS) onboard the Herschel space observatory to study the far-infrared (FIR) properties of submillimeter and optically faint radio galaxies (SMGs and OFRGs). From literature we compiled a sample of 35 securely identified SMGs and nine OFRGs located in the GOODS-N and the A2218 fields. This sample is cross-matched with our PACS 100 m and 160 m multi-wavelength catalogs based on sources-extraction using prior detections at 24 m. About half of the galaxies in our sample are detected in at least the PACS 160 m bandpass. The dust temperatures and the infrared luminosities of our galaxies are derived by fitting their PACS and SCUBA 850 m (only the upper limits for the OFRGs) flux densities with a single modified () black body function. The median dust temperature of our SMG sample is  K while for our OFRG sample it is  K. For both samples, median dust temperatures derived from Herschel data agree well with previous estimates. In particular, Chapman et al. (2005) found a dust temperature of  K for a large sample of SMGs assuming the validity of the FIR/radio correlation (i.e., ). The agreement between our studies confirms that the local FIR/radio correlation effectively holds at high redshift even though we find , a slightly lower value than that observed in local systems. The median infrared luminosities of SMGs and OFRGs are and , respectively. We note that for both samples the infrared luminosity estimates from the radio part of the spectral energy distribution (SED) are accurate, while estimates from the mid-IR are considerably () more uncertain. Our observations confirm the remarkably high luminosities of SMGs and thus imply median star-formation rates of 960 Myr for SMGs with mJy and 460 Myr for SMGs with mJy, assuming a Chabrier IMF and no dominant AGN contribution to the far-infrared luminosity.

1 Introduction

Herschel observations probe the rest-frame far-infrared emission of high-redshift galaxies. Thus, they provide for the first time robust estimates of the infrared luminosities of these high-redshift galaxies and test previous measurements that were based on extrapolation from shorter or longer wavelengths. We here focus on two populations of high-redshift star-forming galaxies selected at submillimeter (submm) and radio wavelengths.
Since their discovery in the late 1990s, submillimeter galaxies (SMGs) have become the selection of choice for the most luminous tail of the high-redshift star-forming galaxy population. It has been found that SMGs have a typical redshift of (Chapman et al., 2005; Pope et al., 2006), are massive systems (, Swinbank et al., 2004; Tacconi et al., 2006) and are compact (e.g., Tacconi et al., 2008). Interferometric observations of their CO molecular gas suggest that the most luminous SMGs ( mJy) are merging sytems (Tacconi et al., 2006, 2008) with high star-formation efficiencies compared to typical galaxies of a similar mass (Daddi et al., 2008). Therefore, these SMGs are thought to exhibit very intense (SFR1000 M yr) short-lived star-formation bursts triggered by mergers and to be the high-redshift progenitors of local massive early-type galaxies (Daddi et al., 2007a, b; Tacconi et al., 2008; Cimatti et al., 2008).
Although SMGs provide a powerful tool to constrain the formation and the evolution of high-redshift dusty star-forming galaxies, their selection is subject to strong biases. In particular, because submm observations probe the blackbody emission of dust in the Rayleigh-Jeans regime, they are strongly anti-correlated with the dust temperature (). For a given infrared luminosity, galaxies with hot dust might fall below the detection limit of current submm instruments. The first observational evidence of a missing population of high-redshift dusty star-forming galaxies with hot dust has been given by Chapman et al. (2004) using a selection of radio-detected but submm-faint galaxies with UV spectra consistent with high-redshift starbursts. These optically faint-radio galaxies (OFRGs) have a comoving volume density (i.e., Mpc at , Chapman et al. 2004), stellar masses and sizes comparable to SMGs, and some have a dust temperature of K (Casey et al., 2009a, b).
While SMGs and OFRGs are an important component of the high-redshift massive galaxy population, many of their fundamental properties still rely on indirect measurements. In particular, direct determinations of SMG dust temperatures were limited (Kovács et al., 2006) because they were not done using rest-frame far-infrared observations on both sides of the peak of the SEDs. More importantly, their infrared luminosites are still debated. Indeed, because theoretical simulations of galaxy evolution have had great difficulties to account for the current inferred luminosities/star-formation rates and number counts (Baugh et al., 2005; Davé et al., 2010), they still question whether these luminosities have been overestimated or whether the IMF is significantly more top-heavy than in the local Universe.
Using deep observations by the Photodetector Array Camera & Spectrometer (PACS; Poglitsch et al. 2010) onboard the Herschel space observatory (Pilbratt et al. 2010) we will have for the first time robust estimates of the dust temperatures and the infrared luminosities of SMGs and OFRGs. Throughout the paper we use a cosmology with , and .

Figure 1: Spectral energy distribution (SED) of one SMG (left) and one OFRG (right). Red diamonds present our PACS measurements while green squares present the multi-wavelength ancillary data taken from the literature (Pope et al., 2006; Casey et al., 2009a, b). The modified blackbody emission () best-fitting the data are shown by solid lines. Dashed lines present the Dale & Helou SED template best-fitting the mid- to far-infrared observations. In the left panel, the blue dotted-dashed line shows the Dale & Helou SED template best-fitting the submm and radio photometries. The inset in each panel shows vs .

2 Observations

In this study we used deep PACS 100 m and 160 m observations of the Great Observatories Origins Deep Survey-North (GOODS-N; ) and the Abell 2218 () fields. These observations were taken as part of the PACS Evolutionary Probe (PEP111http://www.mpe.mpg.de/ir/Research/PEP) guaranteed time key program. The GOODS-N field covers a region of (30 hours), while the deep part of the A2218 field covers a region of (13 hours).
At the resolution of Herschel, all sources in our fields are point sources (i.e. FWHM [] at 100 m [160 m]). Flux densities are hence estimated using a point spread function-fitting technique based on prior source positions detected at 24 m. The use of priors provides a straightforward association between the IRAC, MIPS and PACS sources. Using Monte Carlo simulations we estimate the quality of our PACS 100 m and 160 m catalogs, i.e. photometric error, completeness and contamination as a function of the flux density. In the GOODS-N field our observations reach a limit of  mJy and  mJy at 100 m and 160 m respectively, while in the A2218 field they reach a limit of  mJy and  mJy at 100 m and 160 m respectively.
A complete description of PEP data reduction and sources extraction is given in Appendix A of Berta et al. (2010).

3 Galaxy sample

To obtain a robust measurement of the dust temperature and infrared luminosity of a given galaxy one needs to have an accurate estimate of its redshift. Consequently, we decided to restrict our study to a sample of SMGs and OFRGs with accurate redshift estimates derived from secured radio/mid-infrared identifications (PACS identifications of SMGs are presented in Dannerbauer et al. in prep). In the GOODS-N field, our SMG sample is based on multi-wavelength identifications of SCUBA and AzTEC sources made by Pope et al. (2006)222For GN05, GN07, GN10, GN20 and GN20.2, we used the spectroscopic redshifts revised in Pope et al. (2008) and Daddi et al. (2009a, b). and Chapin et al. (2009), respectively. SMGs with tentative redshifts determined from their IRAC or mid/far-infrared/radio colors were excluded from our sample. Sources with multiple optical counterparts (GN04, GN07, GN19 and GN39) were treated as a single system (i.e. we will use the sum of the radio and mid-infrared flux from the two components when determining their far-infrared properties) because they are all thought to be interacting galaxies (Pope et al., 2006). All these different criteria yield an SMG sample containing 29 sources in the GOODS-N field. In the A2218 field, our SMG sample is assembled from the literature (Kneib et al., 2004; Knudsen et al., 2006, 2008) and contains six lensed sources. Because these galaxies are magnified, their mid-to-far infrared fluxes were de-magnified prior to further analysis using magnification factors from the above references. Among these six lensed sources, three correspond to the same lensed galaxy (SMMJ16359+6612; Kneib et al., 2004). Finally, our OFRG sample is taken from Casey et al. (2009a, b) and contains nine sources, all situated in the GOODS-N field. We note that all but three sources of our entire sample (i.e. SMGs and OFRGs) have spectroscopic redshifts.
The SMG and OFRG samples were cross-matched with our PACS multi-wavelength catalogs using a matching radius of . We detected 19 out of 35 SMGs in at least the PACS 160 m bandpass (17 out of 33 if not multi-counting the 3-component lensed source detected in A2218). The PACS sample is slightly biased towards lower redshift sources because of the positive K-correction : while the median redshift of our parent SMG sample is , the median redshift of our PACS detected SMG sample is . Five out of nine OFRGs have PACS 100 m and 160 m detections. This sample is also slightly biased toward lower redshift () because the OFRG situated at the highest redshift is undetected in our PACS images.
We note that our SMG sample contains sources with , while the most luminous tail of the SMG population, mostly associated with major mergers, is defined using . Below, we will draw our conclusions distinguishing these two populations of SMGs.

Figure 2: Dust temperature-luminosity relation. The filled blue squares and opened blue squares denote SMGs located in the GOODS-N fields with spectroscopic and photometric redshift, respectively. The crosses denote sources which contain an AGN, as indicated by the presence of hard X-rays. The filled green diamonds present SMGs located in the A2218 field (the three data points with correspond to the same lensed galaxy). The filled red circles are from our OFRGs sample. The striped area presents results for SMGs extrapolated by Chapman et al. (2005) from radio and submm data. The Chapman et al. (2003) derivation of the median and interquartile range of the - relation observed at is shown by solid and dashed-dotted lines, linearly extrapolated to .

4 Data analysis

In order to infer the dust temperature of our galaxies we fitted their PACS and SCUBA photometry (only the upper limit for the OFRGs) with a modified blackbody function, with a dust emissivity (see Fig 1). Their total infrared luminosities ([8-1000 m]) were inferred from these best fits using the far-infrared luminosity definition (m]) given by Helou et al. (1988) and a color-correction term (Dale et al., 2001, ).

Figure 3: Submm flux densities as function of the infrared luminosity. The symbols are same as in Fig 2 except for the OFRGs, for which we have only upper limits. The solid and dashed lines show the linear fit to the - relation and the 1 envelop ([mJy]). If we remove the lensed-SMGs of A2218 from the fit, we find a weaker correlation ([mJy]).

We adopted a single dust temperature characterization because studies of IRAS galaxies have demonstrated that this provides an accurate diagnostic of the typical heating condition in their interstellar medium (Desert et al., 1990). While for most of our galaxies this single dust temperature characterization provides a good description of their far-infrared SED, for 6 SMGs, this single dust temperature model yields high values (i.e. ). All these galaxies appear either to be the more distant ones or to exhibit far-infrared colors typical of very cold systems. In both cases, their PACS 100 m flux densities might by contaminated by a hotter dust component. Therefore we excluded their PACS 100 m photometry from the fit and recomputed their dust temperatures. We note that excluding the PACS 100 m photometry from the fit of all our galaxies changes their median dust temperature by only K.
We tested that our results are relatively insensitive to and to our single dust component characterization. Indeed we note that using , we found only small differences in the values of ( K). Moreover, we also note that to fit the PACS and SCUBA photometry with the multiple dust components model of Dale & Helou (2002) yields rest-frame infrared colors (), or equivalently , which excellently agree with those inferred from our blackbody analysis.

5 Discussion

Figure 2 depicts the locations of our SMGs and OFRGs on the - plane and Fig 3 shows their locations on the - plane. As already mentioned, OFRGs are biased towards hot dust temperatures; their median is of  K and their median is . In contrast, SMGs have lower dust temperatures with median  K and . We note that lensed-SMGs from A2218 and with exhibit intermediate dust properties and are less biased towards cold dust temperatures than the entire SMG sample. This is because these galaxies would have escaped both the SMG and OFRG selection method without magnification. We also note that bright SMGs (i.e. ) have higher median infrared luminosities () and higher median dust temperatures ( K) than the entire SMG sample because there is a correlation between and (Fig 3). These estimates are the first direct observational measurements of the dust temperatures and the infrared luminosities of SMGs and OFRGs.
Our observations reveal that high redshift dusty star-forming galaxies exhibit a wide range of dust temperatures. In particular at low infrared luminosities () the dust temperature dispersion observed in our sample might suggest a higher - scatter than that observed by Chapman et al. (2003) at . Nevertheless, this conclusion is most likely driven by selection effects because a significant fraction of the galaxies with intermediate dust properties were probably missed by our current sample. Indeed, we note that studying a -selected sample of galaxies observed with Herschel, Hwang et al. (in prep) find modest changes in the - relation as function of the redshift : at , galaxies with are slightly colder (K) than local ones and the scatter of the - relation slightly increase at high redshift.
Though previous estimates of the dust temperatures of SMGs and OFRGs relied on indirect observations, they agree relatively well with our measurements. In particular, Chapman et al. (2005) found a dust temperature of  K for a large sample of SMGs assuming the validity of the FIR/radio correlation. In order to establish this agreement on a common sample, we applied the same method as Chapman et al. (2005) to our SMG sample, i.e. we fitted the radio and 850 m photometries with dust SED templates from Dale & Helou (2002) and then translated them into using their R(60,100) to map. With this method we found higher (by K) and ( times) than what we obtained using our blackbody analysis. These discrepancies arise because the Dale & Helou SED templates assume a FIR/radio correlation with (Yun et al., 2001), while in our samples we find (see also Ivison et al. 2010, this issue). Although this value of is still in line with results from local systems (which have a dispersion of 0.19 dex), it is also consistent with an evolution of proportional to as found by Ivison et al. (2010).
Our results reveal that one can obtain a very reliable estimate of the infrared luminosity of a given galaxy from its radio flux density ( dex) using . In contrast, the use of the 24 m emission and of the Chary & Elbaz SED library yields an inaccurate estimate of the infrared luminosity characterized by a large scatter ( dex) and a systematic overestimation ( times) of the most luminous galaxies (). We thus find that for the very luminous infrared galaxies studied here, luminosity extrapolations based on the radio emission are considerably more reliable than those based on the mid-infrared emission (see also Elbaz et al. 2010 and Nordon et al. 2010).
Using , we can predict the infrared luminosities of our PACS undetected SMGs. Then, using the Dale & Helou SED templates normalized to these infrared luminosities, we can fit their 850 m photometries. We find that for 13 out of 16 undetected SMGs, PACS flux densities inferred using these fits are below the detection threshold of our observations. Of the three sources with PACS fluxes predictions above our detection threshold, one is known to be contaminated by an AGN and the other two are suspected to have wrong redshift estimates (Daddi et al., 2009b). The PACS nondetections are thus fully consistent with the properties inferred from the detections. This analysis cannot be performed on our PACS undetected OFRGs because they are also undetected at the SCUBA wavelength.

Our observations unambiguously confirm the remarkably large infrared luminosities of bright SMGs (i.e. ) which correspond to SFRs of (SFR , assuming a Chabrier IMF and no dominant AGN contribution to the far-infrared luminosity). Such high SFRs are difficult to reconcile with secular evolution (e.g. Davé et al., 2010) and could correspond to a merger-driven stage in the evolution of these galaxies. This hypothesis is supported by CO observations of bright SMGs which have revealed large CO line-widths and disturbed gas morphologies (Tacconi et al., 2008). Our observations also confirm that OFRGs exhibit higher dust temperatures than faint SMGs () observed at the same redshift and with equivalent infrared luminosities. While the relatively low median SFRs of OFRGs and faint SMGs ( and respectively) could be explained by secular evolution, we need to understand why they exhibit different dust temperatures and to study a possible link with bright SMGs. A clear evolutionary picture will require detailed studies of the dust and molecular gas distribution in a sample of high-redshift star-forming galaxies unbiased towards any particular dust temperature. This SFR-selected sample can now be built with our ongoing deep Herschel observations.

Acknowledgements.
PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, 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/INAF (Italy), and CICYT/MCYT (Spain).

References

  • Baugh et al. (2005) Baugh, C. M., Lacey, C. G., Frenk, C. S., et al. 2005, MNRAS, 356, 1191
  • Berta, S., et al. (2010) Berta, S., et al. 2010, A&A, this Volume
  • Casey et al. (2009a) Casey, C. M., Chapman, S. C., Beswick, R. J., et al. 2009a, MNRAS, 399, 121
  • Casey et al. (2009b) Casey, C. M., Chapman, S. C., Neri, R., et al. 2009b, ArXiv e-prints 0910.5756
  • Chapin et al. (2009) Chapin, E. L., Pope, A., Scott, D., et al. 2009, MNRAS, 398, 1793
  • Chapman et al. (2005) Chapman, S. C., Blain, A. W., Smail, I., & Ivison, R. J. 2005, ApJ, 622, 772
  • Chapman et al. (2003) Chapman, S. C., Helou, G., Lewis, G. F., & Dale, D. A. 2003, ApJ, 588, 186
  • Chapman et al. (2004) Chapman, S. C., Smail, I., Blain, A. W., & Ivison, R. J. 2004, ApJ, 614, 671
  • Cimatti et al. (2008) Cimatti, A., Cassata, P., Pozzetti, L., et al. 2008, A&A, 482, 21
  • Daddi et al. (2007a) Daddi, E., Alexander, D. M., Dickinson, M., et al. 2007a, ApJ, 670, 173
  • Daddi et al. (2008) Daddi, E., Dannerbauer, H., Elbaz, D., et al. 2008, ApJ, 673, L21
  • Daddi et al. (2009a) Daddi, E., Dannerbauer, H., Krips, M., et al. 2009a, ApJ, 695, L176
  • Daddi et al. (2009b) Daddi, E., Dannerbauer, H., Stern, D., et al. 2009b, ApJ, 694, 1517
  • Daddi et al. (2007b) Daddi, E., Dickinson, M., Morrison, G., et al. 2007b, ApJ, 670, 156
  • Dale & Helou (2002) Dale, D. A. & Helou, G. 2002, ApJ, 576, 159
  • Dale et al. (2001) Dale, D. A., Helou, G., Contursi, A., Silbermann, N. A., & Kolhatkar, S. 2001, ApJ, 549, 215
  • Davé et al. (2010) Davé, R., Finlator, K., Oppenheimer, B. D., et al. 2010, MNRAS, 360
  • Desert et al. (1990) Desert, F.-X., Boulanger, F., & Puget, J. L. 1990, A&A, 237, 215
  • Elbaz, D., et al. (2010) Elbaz, D., et al. 2010, A&A, this Volume
  • Helou et al. (1988) Helou, G., Khan, I. R., Malek, L., & Boehmer, L. 1988, ApJS, 68, 151
  • Ivison et al. (2010) Ivison, R. J., Alexander, D. M., Biggs, A. D., et al. 2010, MNRAS, 402, 245
  • Ivison, R. J., Magnelli, B., Ibar, E. et al. (2010) Ivison, R. J., Magnelli, B., Ibar, E. et al. 2010, A&A, this Volume
  • Kneib et al. (2004) Kneib, J., van der Werf, P. P., Kraiberg Knudsen, K., et al. 2004, MNRAS, 349, 1211
  • Knudsen et al. (2006) Knudsen, K. K., Barnard, V. E., van der Werf, P. P., et al. 2006, MNRAS, 368, 487
  • Knudsen et al. (2008) Knudsen, K. K., van der Werf, P. P., & Kneib, J. 2008, MNRAS, 384, 1611
  • Kovács et al. (2006) Kovács, A., Chapman, S. C., Dowell, C. D., et al. 2006, ApJ, 650, 592
  • Nordon, R., et al. (2010) Nordon, R., et al. 2010, A&A, this Volume
  • Pilbratt, G., et al. (2010) Pilbratt, G., et al. 2010, A&A, this Volume
  • Poglitsch, A., et al. (2010) Poglitsch, A., et al. 2010, A&A, this Volume
  • Pope et al. (2008) Pope, A., Chary, R., Alexander, D. M., et al. 2008, ApJ, 675, 1171
  • Pope et al. (2006) Pope, A., Scott, D., Dickinson, M., et al. 2006, MNRAS, 370, 1185
  • Swinbank et al. (2004) Swinbank, A. M., Smail, I., Chapman, S. C., et al. 2004, ApJ, 617, 64
  • Tacconi et al. (2008) Tacconi, L. J., Genzel, R., Smail, I., et al. 2008, ApJ, 680, 246
  • Tacconi et al. (2006) Tacconi, L. J., Neri, R., Chapman, S. C., et al. 2006, ApJ, 640, 228
  • Yun et al. (2001) Yun, M. S., Reddy, N. A., & Condon, J. J. 2001, ApJ, 554, 803

Appendix A Authors’ affiliations

  1. Max-Planck-Institut für Extraterrestrische Physik (MPE), Postfach 1312, 85741 Garching, Germany.

  2. Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/Service d’Astrophysique, Bât.709, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, France.

  3. Herschel Science Centre; European Space Astronomy Centre

  4. ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany.

  5. INAF - Osservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste, Italy.

  6. Instituto de Astrofísica de Canarias, 38205 La Laguna, Spain.

  7. Departamento de Astrofísica, Universidad de La Laguna, Spain.

  8. Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, 40127 Bologna, Italy.

  9. INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy.

  10. INAF - Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy.

  11. Dipartimento di Astronomia, Università di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy.

Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
316118
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description