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Editorial: Understanding the Growth of the First Supermassive Black Holes

Published online by Cambridge University Press:  01 August 2016

Rosa Valiante
Affiliation:
INAF - Osservatorio Astronomico di Roma, via di Frascati 33, 00040, Monteporzio Catone, Italy
Raffaella Schneider
Affiliation:
INAF - Osservatorio Astronomico di Roma, via di Frascati 33, 00040, Monteporzio Catone, Italy
Marta Volonteri
Affiliation:
CNRS, UMR 7095, Institut dAstrophysique de Paris, F-75014, Paris, France
Corresponding
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The formation, assembly history, and environmental impact of the massive black holes (BH) that are ubiquitous in the nuclei of luminous galaxies today remain some of the main unsolved problems in cosmic structure formation. In the last several years, it has become clear that quasars are not just tracers of early and recent structure formation, but that they seem to have actively influenced galaxies and clusters through feedback mechanisms that are still not well understood. The discovery of more and more numerous quasars at redshift above 6, powered by BHs with masses similar to that of their local counterparts, further complicates this scenario. This emphasises the urgent need to better understand how and when such massive objects form and grow, what is the strength and scale of their impact on the evolution of their host galaxies, and what are the main physical processes driving and regulating this co-evolution.

Type
Review Article
Copyright
Copyright © Astronomical Society of Australia 2016 

The formation, assembly history, and environmental impact of the massive black holes (BH) that are ubiquitous in the nuclei of luminous galaxies today remain some of the main unsolved problems in cosmic structure formation. In the last several years, it has become clear that quasars are not just tracers of early and recent structure formation, but that they seem to have actively influenced galaxies and clusters through feedback mechanisms that are still not well understood. The discovery of more and more numerous quasars at redshift above 6, powered by BHs with masses similar to that of their local counterparts, further complicates this scenario. This emphasises the urgent need to better understand how and when such massive objects form and grow, what is the strength and scale of their impact on the evolution of their host galaxies, and what are the main physical processes driving and regulating this co-evolution.

The current challenge for theoretical models and numerical simulations is to predict the formation path to the first z ~ 6 quasars starting from seed BHs, whilst producing a population in agreement with constraints at lower redshift, including the local Universe. At the same time, observations are tackling the difficult task of detecting the rare, faint, and elusive signatures of the first collapsing and merging BHs, such as the highest redshift emission of gamma-ray bursts, X-rays and, perhaps, gravitational waves.

The papers presented in this special issue are a comprehensive review of the most recent theoretical and observational results presented in July 2015 during the European Week of Astronomy and Space Science (EWASS) Symposium 1. This meeting has been an opportunity to bring together some of leader scientists in the field and a unique opportunity to foster discussion on the relevant processes operating on different scales and in different physical regimes relevant to BHs. In this introduction, we summarise the most recent findings and open questions raised during the conference regarding (i) the formation of BH seeds and their early growth to the first, high redshift, supermassive BHs (SMBHs); (ii) the physical properties of the first quasars and the co-evolution of their central SMBHs with the host galaxies; (iii) the observational signatures and local relics of SMBHs suggesting strategies/tracers to observe them with the most sensitive and high resolution future instruments.

It has been widely discussed in the literature that if the growth of the first SMBHs starts from BH remnants of Population III (Pop III) stars, i.e. light seeds with mass ~ 100 M, it requires super-Eddington accretion. An alternative route is to start from the so-called heavy BH seeds, formed by the direct collapse of gas onto a ~ 105 M BH (e.g. Johnson & Haardt Reference Johnson and Haardt2016 for a recent review).

The different channels for BH seeds formation have been presented by several contributors (see the reviews by Volonteri Reference Volonteri2010; Latif & Ferrara Reference Latif and Ferrara2016), with particular emphasis on the formation mechanisms and relevant processes of the so-called direct collapse scenario, from the formation and mass accretion of a supermassive star (SMS) to its collapse to a massive BH. From reviews and contributed talks, it emerged that direct collapse BHs (DCBHs) of 104–106 M (e.g. Ferrara et al. Reference Ferrara, Salvadori, Yue and Schleicher2014), formed by the collapse of gas in massive metal-poor halos exposed to a strong H2 dissociating UV radiation, currently represent the most popular scenario amongst the community working on the first stars. These seeds have been proposed as a viable channel to explain the most luminous quasars (> 1047 erg s−1) observed at z > 6 and the cosmic near infrared and X-ray background cross correlation recently detected (Cappelluti et al. Reference Cappelluti2013).

Andrea Ferrara presented a review on the first stars and BHs in the reionisation era, discussing the physical relation between stars and BHs and their role—as sources of UV photons—for reionisation. In his review, Andrea Ferrara stressed that observations of DCBHs would be a key discovery to interpret the nature of the cosmic infrared background fluctuations excess and its cross correlation with the X-ray cosmic background. However, the abundance of DCBHs is still uncertain because of the uncertain assumptions adopted to compute their birth mass function, such as the value of the critical intensity of the UV flux required for direct collapse to occur.

A DCBH detection method could be through the detection of narrow (≲ 200 km s−1) bright Lyα and He II lines, in absence of metal lines. Very bright (> 1043 erg s−1) Lyα and He II narrow lines have been observed in the brightest Lyα emitter, CR7, at redshift ~ 6.6 (Matthee et al. Reference Matthee, Sobral, Santos, Röttgering, Darvish and Mobasher2015; Sobral et al. Reference Sobral, Matthee, Darvish, Schaerer, Mobasher, Röttgering, Santos and Hemmati2015). It has been proposed that these observed extreme line luminosities can be explained by an accreting DCBH (e.g. Pallottini et al. Reference Pallottini2015; Agarwal et al. Reference Agarwal, Johnson, Zackrisson, Labbe, van den Bosch, Natarajan and Khochfar2015; Hartwig et al. Reference Hartwig, Glover, Klessen, Latif and Volonteri2015; Smith, Bromm, & Loeb Reference Smith, Bromm and Loeb2016; Smidt, Wiggins, & Johnson Reference Smidt, Wiggins and Johnson2016). However, a Pop III galaxy nature of this object cannot be ruled out as such extremely bright lines can be also explained through a recent ≲ 2 Myr PopIII star formation episode (Sobral et al. Reference Sobral, Matthee, Darvish, Schaerer, Mobasher, Röttgering, Santos and Hemmati2015; Visbal, Haiman, & Bryan Reference Visbal, Haiman and Bryan2016; Dijkstra, Gronke, & Sobral Reference Dijkstra, Gronke and Sobral2016). Unfortunately, clear observational signatures to discriminate amongst the two scenarios (accreting DCBH or Pop III stars) are difficult to identify, as suggested also by other contributors.

Kazuyuki Omukai critically discussed the viability of the DCBHs formation pathway, exploring in detail the environmental conditions that trigger or inhibit gas collapse and the subsequent formation of the SMS: intensity of the UV radiation, gas metallicity, gas monolithic collapse or fragmentation and protostellar (continuous or halted) accretion (Omukai & Nishi Reference Omukai and Nishi1999; Omukai Reference Omukai2001; Omukai, Schneider, & Haiman Reference Omukai, Schneider and Haiman2008; Inayoshi & Omukai Reference Inayoshi and Omukai2012; Inayoshi, Omukai, & Tasker Reference Inayoshi, Omukai and Tasker2014). The formation of a SMS and whether or not it becomes massive enough has been widely investigated by numerical simulations that show that it can occur even in the presence of gas fragmentation. However, UV feedback from the growing star itself can halt the accretion rate and plays a crucial role for the subsequent formation of the massive BH seed (e.g. Hosokawa, Omukai, & Yorke Reference Hosokawa, Omukai and Yorke2012; Hosokawa et al. Reference Hosokawa, Yorke, Inayoshi, Omukai and Yoshida2013).

There has been a wide consensus that SMS and thus DCBH formation occurs in very rare environments and that the UV background flux illuminating the gas clouds in the proto-galaxies plays a crucial role. Muhammad Latif highlighted that one of the key parameters for isothermal direct collapse is in fact, the critical value of the UV flux, J crit, required to suppress the formation of H2. He also presented an alternative scenario for BH formation in the presence of a moderate amount of H2 cooling. In particular, Latif & Volonteri (Reference Latif and Volonteri2015) use high-resolution cosmological simulations to study the collapse of massive primordial haloes and the evolution of their dynamical and thermodynamical properties showing that, in some cases, complete isothermal collapse and H2 suppression are not necessary to form a SMS and the large rate required for its efficient accretion (~ 0.1 M yr−1) can be obtained if the halo is illuminated by an external Lyman Werner (LW) radiation of J LW = (500–1000)1021 erg cm2 s1 Hz1 sr1 (Latif & Volonteri Reference Latif and Volonteri2015).

Different contributors stressed the importance of H2 self-shielding that can prevent the direct collapse favouring gas fragmentation (e.g. Glover Reference Glover2015a, Reference Glover2015b and Hartwig et al. Reference Hartwig, Glover, Klessen, Latif and Volonteri2015), magnetic fields that, on the other hand, can suppress gas fragmentation helping the formation of massive objects (Latif et al. Reference Latif, Schleicher, Schmidt and Niemeyer2013a, Reference Latif, Schleicher, Schmidt and Niemeyer2013b, Reference Latif, Schleicher, Bovino and Grassi2014, Reference Latif, Bovino, Van Borm, Grassi, Schleicher and Spaans2014a).

The impact of reionisation on the formation of DCBHs has been discussed by Jarrett Johnson who presented cosmological simulations for the collapse of primordial gas into atomic cooling halos, including the effects of both dissociating (LW) and ionising photons. He showed that ionising radiation triggers the formation of Pop III stars thanks to the rapid formation of H2 molecules, favoured by the presence of a large fraction of free electrons in the ionised gas. The subsequent efficient molecular cooling prevents DCBH formation. However, in atomic cooling halos, the dense gas is self-shielded to ionising photons. As a result, photoionisation has only a moderate effect on DCBH formation (Johnson et al. Reference Johnson, Whalen, Fryer and Li2012, Reference Johnson, Whalen, Agarwal, Paardekooper and Khochfar2014).

Francesco Haardt reviewed the rate at which seed BHs grow, immediately following their formation. This is dictated both by the mechanical and radiative feedback from their progenitor stars and by the impact of the radiation produced in the accretion process itself. If it occurs from a sufficiently dense gas reservoir, short periods of super-Eddington accretion represents an efficient mechanism of BH mass growth. This possibility has been the subject of recent studies whose results have been critically discussed (Volonteri, Silk, & Dubus Reference Volonteri, Silk and Dubus2015; Lupi et al. Reference Lupi, Haardt, Dotti, Fiacconi, Mayer and Madau2016; Pacucci, Volonteri, & Ferrara Reference Pacucci, Volonteri and Ferrara2015; Pezzulli, Valiante, & Schneider Reference Pezzulli, Valiante and Schneider2016). A third hypothesis has been discussed in this review: The formation of an intermediate mass seed BH (103–104 M), through mergers of stars or stellar mass BHs in dense clusters, may give rise to a SMBH. (e.g. Devecchi & Volonteri Reference Devecchi and Volonteri2009, Devecchi et al. Reference Devecchi, Volonteri, Rossi, Colpi and Zwart2012; Lupi et al. Reference Lupi, Colpi, Devecchi, Galanti and Volonteri2014).

Recently, Valiante et al. (Reference Valiante, Schneider, Volonteri and Omukai2016) investigated the role of light and heavy seed BHs in z > 6 SMBHs formation, showing that it strongly depends on the interplay between chemical, radiative, and mechanical feedback effects. They find that Eddington-limited accretion of gas onto few heavy seeds formed at z > 15 can eventually lead to a > 109 M BH.

One of the important aspects in understanding the formation of the first SMBHs, is the study of the properties of their host galaxies. Observations of quasars at high redshift is the key to unveil the environment in which such objects form and evolve.

Xiaohui Fan summarised the recent results on the physical properties of the most luminous quasars in the early Universe. He presented a new survey at high redshift (z = 5–7) based on optical photometry and IR data from UKIDSS and WISE. The new observational techniques allow to expand high-redshift frontiers with more than 200 quasars detected at redshift z > 5 and ~ 100 at redshift z > 6, powered by SMBHs of more than 10 billion solar masses and shining close to the Eddington limit (e.g. Wu et al. Reference Wu2015). An increasing number of fainter quasars has been observed in the last decade, but the quasar density is exponentially declining at z > 6, suggesting that we may be running out of z > 6 quasars. Observations reveal no redshift evolution of the quasar emission and host galaxy metallicity, showing that high-z quasars are old and live in metal-rich environments. However, not all quasars are the same, some of them show very complex gas kinematics that require high sensitivity observations (e.g. with the Atacama Large Millimeter Array, ALMA) to be investigated.

Roberto Maiolino’s review focussed on the observational signatures of AGN (negative/positive) feedback at high redshift and implications for BH-host galaxy co-evolution.

It appeared clear from discussions and talks that there is still no consensus on whether BH growth precedes galaxy assembly or vice versa. Negative feedback has been invoked to prevent the overgrowth of massive galaxies, to explain red-and-dead local massive ellipticals and the BH-stellar mass relation, whilst positive feedback has been proposed to explain the observed specific star-formation rate at high redshift, the strong star-formation efficiency of ultra luminous IR galaxies and sub-millimetre galaxies and as an alternative mechanism for the onset of the BH-stellar mass relation. Roberto Maiolino pointed out that observations of gas outflow, traced by CO and Cii emission lines, suggest that quasar feedback quenching star formation must already be in place in a fraction of massive galaxies at z ~ 6, close to the reionisation epoch. However, tracing cold molecular outflows triggered by AGN, at z > 6, is still very challenging and it has been done only in few bright quasars so far, like SDSSJ1148+5251 in which CO and C ii emission lines are spatially resolved, revealing strong and extended emissions correlated to gas outflows > 2000 Myr−1 (Maiolino et al. Reference Maiolino2012; Cicone et al. Reference Cicone2015) as expected by theoretical models (e.g. Valiante et al. Reference Valiante, Schneider, Maiolino and Salvadori2012). However, whether AGN negative feedback can efficiently quench star formation in galaxies is still unclear. Additional mechanisms have been proposed, such as galaxy strangulation, in which infall of cold gas is somehow halted, but is still not clear what processes inhibit gas accretion (Peng, Maiolino, & Cochrane Reference Peng, Maiolino and Cochrane2015).

On the other hand, observational evidences of positive feedback suggest that star formation may be triggered by quasar-driven winds at high redshift (e.g. Cresci et al. Reference Cresci2015) suggesting that positive feedback may be an important process in galaxy formation as well. Instruments like ALMA and the James Webb Space Telescope (JWST) will provide major progress on this issue.

Invited and contributed talks indeed underlined that high-resolution sub-mm/mm observations may lead to a breakthrough in understanding high-z quasar properties, e.g. with instruments like ALMA which is able to spatially resolve C ii emission out to redshift z > 6, enabling the study of complex gas kinematics and rotating discs.

In addition, whilst it is well known that low-J CO transitions are the best tracer of cold molecular gas in the interstellar and intergalactic medium at high redshift, Simona Gallerani discussed how high-J CO transition lines can be used as a tool to detect high-redshift dust-obscured SMBHs ancestors. She reported the first, serendipitous, detection of the CO(17–16) emission line in the best studied quasar SDSS J1148+5251 at z = 6.4 obtained with the Plateau de Bure Interferometer. Models suggest that X-ray dominated regions are required to reproduce such high luminosity line (Gallerani et al. Reference Gallerani, Ferrara, Neri and Maiolino2014).

Together with high-sensitive, high-resolution observations, theoretical models have a fundamental role in the study of the formation and evolution of the first SMBHs. Tiziana Di Matteo and Yohan Dubois introduced the current advances in numerical simulations aimed to study the rapid growth of BHs at high redshift and their co-evolution with the host galaxy (e.g. Dubois, Volonteri, & Silk Reference Dubois, Volonteri and Silk2014). A large number of semi-analytic models and simulations have been developed to date, with the most updated numerical techniques. In particular, current numerical simulations are growing in size and resolution being able to resolve the full mass function from dwarf galaxies to super clusters of galaxies (e.g. Feng et al. Reference Feng, Di Matteo, Croft, Tenneti, Bird, Battaglia and Wilkins2015). One of the aims of theoretical models is to study BH-host galaxy scaling relations, such as the BH-stellar bulge mass correlation, explaining how and when such relations sets in.

The best observational signatures to constrain the origin of the first SMBHs were discussed during the meeting. The detection of the first massive BHs (105 − 107 M) at high redshift would provide unique constraints on the MBH formation mechanism and subsequent growth. Optical, IR, X-ray, and radio searches for BHs in dwarf galaxies and the observations of distant X-ray loud and radio galaxies have been proposed as some of the most promising tools by several contributors.

Amy Reines presented ongoing efforts to search for and study the smallest BHs in present-day dwarf galaxies, which are beginning to provide the much needed observational constraints on the masses, host galaxies, and formation path of SMBH seeds. From the first systematic search for AGNs in dwarf galaxies (Reines, Greene, & Geha Reference Reines, Greene and Geha2013), an increasing number of dwarf galaxies with optical signatures of active massive BHs have been identified. These reveal the least massive BHs known so far, ~ 105 − 104 M, such as the one in the nucleus of RGG 118 (Baldassare et al. Reference Baldassare, Reines, Gallo and Greene2015). However, only ~ 0.5% of dwarf galaxies present optical signatures of accreting massive BHsFootnote 1 and thus other diagnostic tools are required, such as X-ray, MIR, and radio observations. The first example of a dwarf starburst galaxy with a massive BH (~ 2 × 106 M) has been revealed by means of joint optical (HST), radio (VLA), and X-ray (CXO) observations in the galaxy Heinze 2–10 (Reines et al. Reference Reines, Sivakoff, Johnson and Brogan2011; Reines & Deller Reference Reines and Deller2012).

Finally, Andrea Comastri emphasised the important role of high energy X-ray observations to reveal the dominant obscured AGN population (more than 50% of z > 3 AGN are heavily obscured), presenting the most recent deep XMM and Chandra surveys probing the z ~ 3–6 Universe and discussing the expectations and observational strategies for the future surveys with eROSITA and ATHENA Wide Field Imager (WFI). The latter is expected to provide breakthroughs in the determination of the luminosity function and its evolution up to very high redshift (z > 6 [Aird et al. Reference Aird2013]).

As organisers of the EWASS 2015 symposium—entitled Understanding the growth of the first SMBHs—we asked the invited speakers to contribute to this issue with original papers reviewing the results and fruitful discussions presented during the symposium. We thank the EWASS 2015 organisers for giving us the opportunity to hold an interesting meeting in the beautiful island of Tenerife.

Footnotes

1 Such an active occupation fraction translates into a lower limit to the occupation fraction of ~ 20% Miller et al. (Reference Miller, Gallo, Greene, Kelly, Treu, Woo and Baldassare2015).

References

Agarwal, B., Johnson, J. L., Zackrisson, E., Labbe, I., van den Bosch, F. C., Natarajan, P., & Khochfar, S. 2016, MNRAS, 460, 4003 10.1093/mnras/stw1173 mnras.oxfordjournals.org/content/460/4/4003 CrossRefGoogle Scholar
Aird, J., et al. 2013, arXiv: 1306.2325arxiv.org/abs/1306.2325 Google Scholar
Baldassare, V. F., Reines, A. E., Gallo, E., & Greene, J. E. 2015, ApJ, 809, L14 10.1088/2041-8205/809/1/L14 2015ApJ...1809L..14B CrossRefGoogle Scholar
Cappelluti, N., et al. 2013, ApJ, 769, 68 10.1088/0004-637X/769/1/68 2013ApJ...769...68C CrossRefGoogle Scholar
Cicone, C., et al. 2015, A&A, 574, A14 10.1051/0004-6361/201424980 2015A&A...574A..14C Google Scholar
Cresci, G., et al. 2015, A&A, 582, A63 10.1051/0004-6361/201526581 2015A&A...582A..63C Google Scholar
Devecchi, B., & Volonteri, M. 2009, ApJ, 694, 302 CrossRefGoogle Scholar
Devecchi, B., Volonteri, M., Rossi, E. M., Colpi, M., Portegies Zwart, S. 2012, MNRAS, 421, 1465 CrossRefGoogle Scholar
Dijkstra, M., Gronke, M., & Sobral, D. 2016, ApJ, 823, 73 10.3847/0004-637X/823/2/74 adsabs.harvard.edu/abs/2016ApJ...823...74D CrossRefGoogle Scholar
Dubois, Y., Volonteri, M., & Silk, J. 2014, MNRAS, 440, 1590 10.1093/mnras/stu373 2014MNRAS.440.1590D CrossRefGoogle Scholar
Feng, Y., Di Matteo, T., Croft, R., Tenneti, A., Bird, S., Battaglia, N., & Wilkins, S. 2015, ApJ, 808, L17 10.1088/2041-8205/808/1/L17 2015ApJ...808L..17F CrossRefGoogle Scholar
Ferrara, A., Salvadori, S., Yue, B., & Schleicher, D. 2014, MNRAS, 443, 2410 10.1093/mnras/stu1280 2014MNRAS.443.2410F CrossRefGoogle Scholar
Gallerani, S., Ferrara, A., Neri, R., & Maiolino, R. 2014, MNRAS, 445, 2848 10.1093/mnras/stu2031 2014MNRAS.445.2848G CrossRefGoogle Scholar
Glover, S. C. O. 2015a, MNRAS, 451, 2082 10.1093/mnras/stv1059 2015MNRAS.451.2082G CrossRefGoogle Scholar
Glover, S. C. O. 2015b, MNRAS, 453, 2901 10.1093/mnras/stv1781 2015MNRAS.453.2901G CrossRefGoogle Scholar
Hartwig, T., Glover, S. C. O., Klessen, R. S., Latif, M. A., & Volonteri, M. 2015, MNRAS, 452, 1233 10.1093/mnras/stv1368 2015MNRAS.452.1233H CrossRefGoogle Scholar
Hosokawa, T., Omukai, K., & Yorke, H. W. 2012, ApJ, 756, 93 10.1088/0004-637X/756/1/93 2012ApJ...756...93H CrossRefGoogle Scholar
Hosokawa, T., Yorke, H. W., Inayoshi, K., Omukai, K., & Yoshida, N. 2013, ApJ, 778, 178 10.1088/0004-637X/778/2/178 2013ApJ...778..178H CrossRefGoogle Scholar
Inayoshi, K., & Omukai, K. 2012, MNRAS, 422, 2539 10.1111/j.1365-2966.2012.20812.x 2012MNRAS.422.2539I CrossRefGoogle Scholar
Inayoshi, K., Omukai, K., & Tasker, E. 2014, MNRAS, 445, L109 10.1093/mnrasl/slu151 2014MNRAS.445L.109I CrossRefGoogle Scholar
Johnson, J. L., & Haardt, F. 2016, PASA, 33, e007 10.1017/pasa.2016.4 2016PASA...33....7J CrossRefGoogle Scholar
Johnson, J. L., Whalen, D. J., Agarwal, B., Paardekooper, J.-P., & Khochfar, S. 2014, MNRAS, 445, 686 10.1093/mnras/stu1676 2014MNRAS.445..686J CrossRefGoogle Scholar
Johnson, J. L., Whalen, D. J., Fryer, C. L., & Li, H. 2012, ApJ, 750, 66 10.1088/0004-637X/750/1/66 2012ApJ...750...66J CrossRefGoogle Scholar
Latif, M. A., Bovino, S., Van Borm, C., Grassi, T., Schleicher, D. R. G., & Spaans, M. 2014a, MNRAS, 443, 1979 10.1093/mnras/stu1230 2014MNRAS.443.1979L CrossRefGoogle Scholar
Latif, M. A., & Ferrara, A. 2016, arXiv: 1605.07391arxiv.org/abs/1605.07391 Google Scholar
Latif, M. A., Schleicher, D. R. G., Bovino, S., Grassi, T., & Spaans M. 2014b, ApJ, 792, 78 10.1088/0004-637X/792/1/78 2014ApJ...792...78L CrossRefGoogle Scholar
Latif, M. A., Schleicher, D. R. G., Schmidt, W., & Niemeyer, J. 2013a, MNRAS, 433, 1607 10.1093/mnras/stt834 2013MNRAS.433.1607L CrossRefGoogle Scholar
Latif, M. A., Schleicher, D. R. G., Schmidt, W., & Niemeyer, J. C. 2013b, MNRAS, 436, 2989 10.1093/mnras/stt1786 2013MNRAS.436.2989L CrossRefGoogle Scholar
Latif, M. A., & Volonteri, M. 2015, MNRAS, 452, 1026 10.1093/mnras/stv1337 2015MNRAS.452.1026L CrossRefGoogle Scholar
Lupi, A., Colpi, M., Devecchi, B., Galanti, G., & Volonteri, M. 2014, MNRAS, 442, 3616 10.1093/mnras/stu1120 2014MNRAS.442.3616L CrossRefGoogle Scholar
Lupi, A., Haardt, F., Dotti, M., Fiacconi, D., Mayer, L., & Madau, P. 2016, MNRAS, 456, 2993 10.1093/mnras/stv2877 2016MNRAS.456.2993L CrossRefGoogle Scholar
Maiolino, R., et al. 2012, MNRAS, 425, L66 10.1111/j.1745-3933.2012.01303.x 2012MNRAS.425L..66M CrossRefGoogle Scholar
Matthee, J., Sobral, D., Santos, S., Röttgering, H., Darvish, B., & Mobasher, B. 2015, MNRAS, 451, 400 10.1093/mnras/stv947 2015MNRAS.451..400M CrossRefGoogle Scholar
Miller, B. P., Gallo, E., Greene, J. E., Kelly, B. C., Treu, T., Woo, J.-H., & Baldassare, V. 2015, ApJ, 799, 98 10.1088/0004-637X/799/1/98 2015ApJ...799...98M CrossRefGoogle Scholar
Omukai, K. 2001, ApJ, 546, 635 10.1086/318296 2001ApJ...546..635O CrossRefGoogle Scholar
Omukai, K., & Nishi, R. 1999, ApJ, 518, 64 10.1086/307285 1999ApJ...518...64O CrossRefGoogle Scholar
Omukai, K., Schneider, R., & Haiman, Z. 2008, ApJ, 686, 801 10.1086/591636 2008ApJ...686..801O CrossRefGoogle Scholar
Pacucci, F., Volonteri, M., & Ferrara, A. 2015, MNRAS, 452, 1922 10.1093/mnras/stv1465 2015MNRAS.452.1922P CrossRefGoogle Scholar
Pallottini, A., et al. 2015, MNRAS, 453, 2465 10.1093/mnras/stv1795 2015MNRAS.453.2465P Google Scholar
Peng, Y., Maiolino, R., & Cochrane, R. 2015, Natur, 521, 192 10.1038/nature14439 2015Natur.521..192P CrossRefGoogle Scholar
Pezzulli, E., Valiante, R., & Schneider, R. 2016, MNRAS 10.1093/mnras/stw505 2016MNRAS.tmp..296P Google Scholar
Reines, A. E., & Deller, A. T. 2012, ApJ, 750, L24 10.1088/2041-8205/750/1/L24 2012ApJ...750L..24R CrossRefGoogle Scholar
Reines, A. E., Greene, J. E., & Geha, M. 2013, ApJ, 775, 116 10.1088/0004-637X/775/2/116 2013ApJ...775..116R CrossRefGoogle Scholar
Reines, A. E., Sivakoff, G. R., Johnson, K. E., & Brogan, C. L. 2011, Nature, 470, 66 10.1038/nature09724 2011Natur.470...66R CrossRefGoogle Scholar
Smidt, J., Wiggins, B. K., & Johnson, J. L. 2016, arXiv:1603.00888arxiv.org/abs/1603.00888 Google Scholar
Smith, A., Bromm, V., & Loeb, A. 2016, arXiv:1692.07639arxiv.org/abs/1692.07639 Google Scholar
Sobral, D., Matthee, J., Darvish, B., Schaerer, D., Mobasher, B., Röttgering, H. J. A., Santos, S., & Hemmati, S. 2015, ApJ, 808, 139 10.1088/0004-637X/808/2/139 2015ApJ...808..139S CrossRefGoogle Scholar
Valiante, R., Schneider, R., Maiolino, R., Salvadori, S., & Bianchi S. 2012, MNRAS, 427, L60 10.1111/j.1745-3933.2012.01345.x 2012MNRAS.427L..60V Google Scholar
Valiante, R., Schneider, R., Salvadori, S., & Gallerani, S. 2014, MNRAS, 444, 2442 10.1093/mnras/stu1613 2014MNRAS.444.2442V CrossRefGoogle Scholar
Valiante, R., Schneider, R., Volonteri, M., & Omukai, K. 2016, MNRAS, 457, 3356 10.1093/mnras/stw225 2016MNRAS.457.3356V CrossRefGoogle Scholar
Visbal, E., Haiman, Z., & Bryan, G. L. 2016, MNRAS, 460, L59 10.1093/mnrasl/slw071 adsabs.harvard.edu/abs/2016MNRAS.460L..59V CrossRefGoogle Scholar
Volonteri, M. 2010, ARA&A, 18, 279 10.1007/s00159-010-0029-x 2010A&ARv..18..279V Google Scholar
Volonteri, M., Silk, J., & Dubus, G. 2015, ApJ, 804, 148 10.1088/0004-637X/804/2/148 2015ApJ...804..148V CrossRefGoogle Scholar
Wu, X.-B., et al. 2015, Nature, 518, 512 10.1038/nature14241 2015Natur.518..512W CrossRefGoogle Scholar
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Editorial: Understanding the Growth of the First Supermassive Black Holes
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Editorial: Understanding the Growth of the First Supermassive Black Holes
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Editorial: Understanding the Growth of the First Supermassive Black Holes
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