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Single PDF of All Proposals Yale Observing Proposal Standard proposal Semester: 2014B Date: March 11, 2014 Constraining SMBH growth in the high-redshift Uni- verse PI: Francesca Civano Status: P Affil.: Yale University Physics, P.O. Box 208120, New Haven, CT 06520-8120 U.S.A. Email: [email protected] Phone: 203-432-3651 FAX: 203-432-8552 CoI: Meg Urry Status: P Affil.: Yale University CoI: Stephanie LaMassa Status: P Affil.: Yale University CoI: Benny Trakhtenbrot Status: P Affil.: ETH CoI: Stefano Marchesi Status: G Affil.: Yale University Abstract of Scientific Justification (will be made publicly available for accepted proposals): We propose to measure accurate super massive black hole (SMBH) masses and growth rates 46 (L/LEdd) for a sample of 9 faint (LBol ∼10 erg/s), X-ray-selected Active Galactic Nuclei (AGN) at z ∼ 3.1 − 3.7, from the COSMOS field. Using MOSFIRE, we will not only observe the broad Hβ emission lines in AGN spectra but we will also observe a comparison sample of 15 to 25 epoch- matched galaxies in the same fields, to characterize the SMBH and galaxy growth environment. The COSMOS deep multiwavelength survey probes the growth of SMBHs and their co-evolution with galaxies, at luminosities and redshifts where most black hole and stellar growth occurs. The COSMOS dataset is matched in wavelength coverage in only one or two other fields (which sample at least an order of magnitude smaller in volume), and in particular, the recently awarded Chandra COSMOS Legacy Survey enables a census of SMBH growth from z=0 to z=5 that is nearly unbi- ased by obscuration. Together with the masses and growth rates successfully measured for 6 X-ray selected AGN observed during 2013B in the same COSMOS field, we will have the first sample (15 sources), comparable in size to previous studies at brighter luminosities, in a a parameter (LBol, mass and L/LEdd) space at this critical epoch which has been explored just by our group. The proposed MOSFIRE spectroscopy, combined with the full COSMOS data set, allows direct esti- mates of black hole mass and growth rate (Eddington ratio, Fig. 1) and host galaxy stellar content, directly constraining how SMBHs and galaxies co-evolve. Summary of observing runs requested for this project Run Telescope Instrument No. Nights Min. Nights Moon Optimal months Accept. months 1 Keck MOSFIRE 3 3 dark/grey January 2 3 4 5 Scheduling constraints and non-usable dates (up to four lines). —————————————————— Yale Proposal Page 2 This box blank. Scientific Justification Be sure to include overall significance to astronomy. Limit text to one page with figures, captions and references on no more than two additional pages. Black holes grow and radiate across a wide range of luminosities, and stars form and evolve in galaxies with nearly as broad a range in mass. The large uncertainties on AGN population synthesis and evolution models (Gilli et al. 2007, Treister et al. 2012) demonstrate the importance of measuring SMBH growth across a wide mass-luminosity range. Simply studying optically-selected luminous quasars, for example, accounts for less than 50% of total BH growth (e.g., Treister et al. 2012), and takes place in fewer than 10% of galaxies. Most SMBHs are growing at moderate Eddington rates in moderate luminosity AGN, so measuring the BH mass function across a range of AGN luminosities is clearly critical. This is why a “wedding cake” combination of surveys with different depths and areas is essential to understanding the co-evolution of SMBHs and galaxies. The COSMOS survey, to which an unprecedented 2.8 Ms of Chandra GO time has recently been allocated (PI: Civano), is ideal for sampling the youthful growth period of SMBHs at z > 3 and 44 galaxies near L∗ or just above. Typical COSMOS AGN have LX ∼ 5 × 10 erg/s and reside in 13 haloes with mass M ∼ few × 10 M⊙ at z=3 (Allevato et al. 2014 submitted): if AGN feedback is important for galaxy evolution, these are the SMBHs and galaxies that matter – yet very little is known about them. First estimates of z > 3 AGN luminosity functions measured at X-ray (Civano et al. 2011) and optical wavelengths (Glikman et al. 2011, Ikeda et al. 2011) are inconsistent, but current samples are small and largely disjoint in luminosity or halo mass. Furthermore, the optical bias toward high luminosities and against obscuration implies severe uncertainties in the SMBH growth and evolution during the early ages of the Universe (Trakhtenbrot et al. 2011, Fig. 1). Phenomenological models diverge by up to a factor 10 (Aird et al. 2010, Gilli et a. 2007) and physical models of quasar evolution (Wyithe & Loeb 2009, Shen 2009) are even less constrained. We propose to measure BH masses and growth rates (L/LEdd) for a new sample of 9 faint, X-ray- selected AGN at z ∼ 3.1 − 3.7, from the Chandra COSMOS Legacy Survey. Using MOSFIRE, we will observe the broad Hβ emission line in AGN spectra and also probe stellar properties in galaxies at the same redshifts of the AGN, to characterize the SMBH and galaxy growth environment (see Technical Description). This is the extension of a study started in 2013B (January 2014) when we observed 6 other X-ray selected AGN in the inner region of the COSMOS field (Fig. 2). Feedback models imply that virtually all z>3 large scale structures should host rapidly growing SMBHs, which can shut off the formation of new stars in massive galaxies at z∼2.5 (Benson et al. 2003, Croton et al. 2006). COSMOS AGN at z ∼ 3 are closer in luminosity to the optically-selected samples, and are roughly a decade above the typical AGN luminosities in the Chandra Deep Fields (Civano et al. 2011), so they fill a missing link in BH mass-dependent density evolution. Being hard X-ray-selected, these COSMOS AGN are also almost unbiased with respect to obscuration, so that the SMBH census is far more complete than optical samples; this means we can derive the completeness correction needed for optically-selected AGN. At the early times, the progenitors of lower-redshift structures are made up of many connected overdensities on a scale of several arcminutes (Springel et al. 2005, Overzier et al. 2009), so the MOSFIRE FOV is well suited to identifying and characterizing the members of these structures. Using the unique capabilities (sensitivity and multi-object mode) of MOSFIRE, the proposed ob- servations will enable (1) the study of accretion at z > 3 in a critical luminosity range, fainter than the optically selected quasar samples (Fig. 1), (2) the exploration of the role of accreting SMBHs in their environment and the properties of the galaxies surrounding them, and (3) the comparison with SMBH accretion models and simulations of structure formation (Natarajan & Volonteri 2012). Yale Proposal Page 3 This box blank. Bibliography: Aird et al. 2010, MNRAS 401, 2531; Baskin & Laor, 2005, MNRAS, 356, 1029; Benson et al. 2003, ApJ 599, 38; Croton et al. 2006, MNRAS 365, 11; Civano et al. 2011, ApJ 741, 91; Glikman et al. 2011, ApJL 728, 26; Gilli et al. 2007, A&A 463, 79; Ikeda et al.2011, ApJ 728, 25; Kaspi et al. 2005, ApJ, 629, 61; Kurk et al. 2007, ApJ, 669, 32; McConnell et al. 2011, Nature, 480, 215; Netzer et al. 2007, ApJ, 671, 1256; Natarajan, P., & Volonteri, M. 2012, MNRAS, 422, 2051; Overzier et al. 2009, ApJ 704, 548; Shen et al. 2008, ApJ, 680, 189; Shen 2009, ApJ 704, 89; Springel et al. 2005, Nature 435, 629; Trakhtenbrot et al. 2011, ApJ, 730, 7; Trakhtenbrot & Netzer, 2012, MNRAS, 427, 3081; Vestergaard & Peterson, 2006, ApJ, 641, 689; Volonteri 2010, A&ARv,18, 279; Willott et al. 2010, AJ, 140, 546; Wyithe & Loeb 2009, MNRAS, 395, 1607. 2 2.5 3 3.5 4 4.5 5 5.5 6 6.5 " 48 1 − erg s 47 / Bol L 46 ! log 45 ) ⊙ 10 /M BH 9 M log ( 8 ) Edd 0 /L Bol −1 L −2 log ( 2 2.5 3 3.5 4 4.5 5 5.5 6 6.5 z Figure 1: Bolometric luminosity distribution (top panel), measured by integrating the observed spectral energy distribution, for the nine sources proposed here (red circles), for two sources in the 2013B sample (blue solid squares), compared with the data presented in Trakhtenbrot et al. (2011, black symbols). The measured BH mass and Eddington ratio for the 2013B sources are plotted in the middle and bottom panel. Assuming that the proposed sources have a similar Eddington ratio or BH mass to the Netzer et al. (2007) z ∼3.3 sample (black triangle), we derive their expected masses (middle panel) and ratio (bottom panel). Yale Proposal Page 4 This box blank. 0.6 CID−113: z=3.333 , K =19.95 AB 0.5 log M =8.82, L/L =0.20 /A] BH Edd 2 0.4 erg/s/cm 0.3 −17 0.2 [10 λ F 0.1 0 4500 4600 4700 4800 4900 5000 5100 5200 rest−frame wavelength [A] CID−413: 0.3 z=3.345 , K =20.5 AB log M =8.46, L/L =0.15 /A] BH Edd 2 0.25 0.2 erg/s/cm 0.15 −17 [10 0.1 λ F 0.05 0 4500 4600 4700 4800 4900 5000 5100 5200 rest−frame wavelength [A] Figure 2: MOSFIRE spectra of two out of 6 (plus 1 in CDFS) 2013B sources. The two spectra are plotted in the rest frame. The spectrum (blue line) is shown with the best fit model (black solid) and each component used in the fit (black dashed lines).
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