No Significant Evolution of Relations between Black Hole Mass and Galaxy Total Stellar Mass Up to z ∼ 2.5

Suh, Hyewon; Civano, F.; Trakhtenbrot, Benny; Shankar, Francesco; Hasinger, G.; Sanders, D. B.; Allevato, V.

doi:10.3847/1538-4357/ab5f5f

Cited by 97 publications

(129 citation statements)

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“…Our analysis adds key evidence, using IR data, to an increasing body of work (Delvecchio et al 2019;Ding et al 2020;Shankar et al 2020;Suh et al 2020) on the weak evolution in the BHAR/SFR and its relatively low normalization relative to local raw dynamical M BH − M * relations.…”

Section: Relation Between Stellar Mass and Black Hole Masssupporting

confidence: 54%

Coevolution of black hole accretion and star formation in galaxies up to z = 3.5

Carraro

Rodighiero

Cassata

et al. 2020

A&A

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Aims. We study the coevolution between the black hole accretion rate (BHAR) and the star formation rate (SFR) in different phases of galaxy life: main-sequence star-forming galaxies, quiescent galaxies, and starburst galaxies at different cosmic epochs. Methods. We exploited the unique combination of depth and area in the COSMOS field and took advantage of the X-ray data from the Chandra COSMOS-Legacy survey and the extensive multiwavelength ancillary data presented in the COSMOS2015 catalog, including in particular the UVista Ultra-deep observations. These large datasets allowed us to perform an X-ray stacking analysis and combine it with detected sources in a broad redshift interval (0.1 < z < 3.5) with unprecedented statistics for normal star-forming, quiescent, and starburst galaxies. The X-ray luminosity was used to predict the black holeAR, and a similar stacking analysis on far-infrared Herschel maps was used to measure the corresponding obscured SFR for statistical samples of sources in different redshifts and stellar mass bins. Results. We focus on the evolution of the average SFR-stellar mass (M*) relation and compare it with the BHAR-M* relation. This extends previous works that pointed toward the existence of almost linear correlations in both cases. We find that the ratio between BHAR and SFR does not evolve with redshift, although it depends on stellar mass. For the star-forming populations, this dependence on M* has a logarithmic slope of ∼0.6 and for the starburst sample, the slope is ∼0.4. These slopes are both at odds with quiescent sources, where the dependence remains constant (log(BHAR/SFR) ∼ −3.4). By studying the specific BHAR and specific SFR, we find signs of downsizing for M* and black hole mass (MBH) in galaxies in all evolutionary phases. The increase in black hole mass-doubling timescale was particularly fast for quiescents, whose super-massive black holes grew at very early times, while accretion in star-forming and starburst galaxies continued until more recent times. Conclusions. Our results support the idea that the same physical processes feed and sustain star formation and black hole accretion in star-forming galaxies while the starburst phase plays a lesser role in driving the growth of the supermassive black holes, especially at high redshift. Our integrated estimates of the M* − MBH relation at all redshifts are consistent with independent determinations of the local M* − MBH relation for samples of active galactic nuclei. This adds key evidence that the evolution in the BHAR/SFR is weak and its normalization is relatively lower than that of local dynamical M* − MBH relations.

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Section: Relation Between Stellar Mass and Black Hole Masssupporting

confidence: 54%

Coevolution of black hole accretion and star formation in galaxies up to z = 3.5

Carraro

Rodighiero

Cassata

et al. 2020

A&A

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“…2). Moreover, our data points lie close to the fit recently found by Suh et al (2020) by including local plus highz (up to z=2.5) AGN and to the unbiased M BH − M relation computed by Shankar et al (2016), who interpreted the discrepancy between the observed location of quiescient and active galaxies in the M BH − M plane as an observational bias (Shankar et al 2019). Indeed, our newly discovered z ∼ 1.6 AGN have M BH /M ratio consistent with local active galaxies, thus showing no or negligible evolution in the intrinsic M BH − M relation, in agreement with most recent works (Shankar et al 2019;Suh et al 2020).…”

Section: The M Bh − M Planesupporting

confidence: 90%

“…Correlations between central black hole mass and host galaxy total stellar mass for the two broad line AGN discovered in the core of XDCP004 (black circles with errors). As reference, the dashed red line is a linear fit to the sample of Kormendy & Ho (2013, KH13) by Shankar et al (2019), while the solid green line is the fit to local AGN by Reines & Volonteri (2015, RV15) and the short-dashed blu line is the fit by Suh et al (2020) to local + high-z AGN. Finally the solid black line is the de-biased MBH − M relation derived by Shankar et al (2016, S+16) with its scatter (yellow area).…”

Section: Agn and Sf Activitymentioning

confidence: 99%

The role of AGN activity in the building up of the BCG at z ∼ 1.6

Bongiorno

Travascio

2019

Proc. IAU

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XDCPJ0044.0-2033 is one of the most massive galaxy cluster at z ∼1.6, for which a wealth of multi-wavelength photometric and spectroscopic data have been collected during the last years. I have reported on the properties of the galaxy members in the very central region (∼ 70kpc × 70kpc) of the cluster, derived through deep HST photometry, SINFONI and KMOS IFU spectroscopy, together with Chandra X-ray, ALMA and JVLA radio data.In the core of the cluster, we have identified two groups of galaxies (Complex A and Complex B), seven of them confirmed to be cluster members, with signatures of ongoing merging. These galaxies show perturbed morphologies and, three of them show signs of AGN activity. In particular, two of them, located at the center of each complex, have been found to host luminous, obscured and highly accreting AGN (λ = 0.4−0.6) exhibiting broad Hα line. Moreover, a third optically obscured type-2 AGN, has been discovered through BPT diagram in Complex A. The AGN at the center of Complex B is detected in X-ray while the other two, and their companions, are spatially related to radio emission. The three AGN provide one of the closest AGN triple at z > 1 revealed so far with a minimum (maximum) projected distance of 10 kpc (40 kpc). The discovery of multiple AGN activity in a highly star-forming region associated to the crowded core of a galaxy cluster at z ∼ 1.6, suggests that these processes have a key role in shaping the nascent Brightest Cluster Galaxy, observed at the center of local clusters. According to our data, all galaxies in the core of XDCPJ0044.0-2033 could form a BCG of M* ∼ 1012Mȯ hosting a BH of 2 × 108−109Mȯ, in a time scale of the order of 2.5 Gyrs.

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“…Since the stellar mass evolves much more modestly than the black hole mass [a trend also found in recent AGN observations from the Chandra-COSMOS Legacy Survey; Ref. 15], the central black hole mass makes up a much larger fraction of the stellar mass at high redshifts (a fraction of ∼ 0.3 at redshift z ∼ 6 compared to 10 −4 at z ∼ 0). This fact, whose validity has been hinted at in the past [11,16], is well-supported by the recent ALM A 1 spectroscopic study [10] of [CII]-detected quasars at z > 6 which indicates significantly more than two orders of magnitude evolution of the locally observed black hole -bulge mass relation [7].…”

Section: Introductionmentioning

confidence: 76%

It is feasible to directly measure black hole masses in the first galaxies

Padmanabhan

Loeb

2020

J. Cosmol. Astropart. Phys.

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In the local universe, black hole masses have been inferred from the observed increase in the velocities of stars at the centres of their host galaxies. So far, masses of supermassive black holes in the early universe have only been inferred indirectly, using relationships calibrated to their locally observed counterparts. Here, we use the latest observational constraints on the evolution of stellar masses in galaxies to predict, for the first time, that the region of influence of a central supermassive black hole at the epochs where the first galaxies were formed is directly resolvable by current and upcoming telescopes. We show that the existence of the black hole can be inferred from observations of the gas or stellar disc out to > 0.5 kpc from the host halo at redshifts z 6. Such measurements will usher in a new era of discoveries unraveling the formation of the first supermassive black holes based on subarcsecond-scale spectroscopy with the JW ST , ALM A, and the SKA. The measured mass distribution of black holes will allow forecasting of the future detection of gravitational waves from the earliest black hole mergers.

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No Significant Evolution of Relations between Black Hole Mass and Galaxy Total Stellar Mass Up to z ∼ 2.5

Cited by 97 publications

References 99 publications

Coevolution of black hole accretion and star formation in galaxies up to z = 3.5

Coevolution of black hole accretion and star formation in galaxies up to z = 3.5

The role of AGN activity in the building up of the BCG at z ∼ 1.6

It is feasible to directly measure black hole masses in the first galaxies

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