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1. KASHz+SUPER: Evidence of cold molecular gas depletion in AGN hosts at cosmic noon.

Author

Bertola, E., Circosta, C., Ginolfi, M., Mainieri, V., Vignali, C., Calistro Rivera, G., Ward, S. R., Lopez, I. E., Pensabene, A., Alexander, D. M., Bischetti, M., Brusa, M., Cappi, M., Comastri, A., Contursi, A., Cicone, C., Cresci, G., Dadina, M., D'Amato, Q., and Feltre, A.

Subjects
ACTIVE galaxies, GALACTIC evolution, GAS reservoirs, GAS distribution, COLD gases, ACTIVE galactic nuclei
Abstract

The energy released by active galactic nuclei (AGN) has the potential to heat or remove the gas of the ISM, thus likely impacting the cold molecular gas reservoir of host galaxies at first, with star formation following as a consequence on longer timescales. Previous works on high-z galaxies, which compared the gas content of those without identified AGN, have yielded conflicting results, possibly due to selection biases and other systematics. To provide a reliable benchmark for galaxy evolution models at cosmic noon (z = 1 − 3), two surveys were conceived: SUPER and KASHz, both targeting unbiased X-ray-selected AGN at z > 1 that span a wide bolometric luminosity range. In this paper we assess the effects of AGN feedback on the molecular gas content of host galaxies in a statistically robust, uniformly selected, coherently analyzed sample of AGN at z = 1 − 2.6, drawn from the KASHz and SUPER surveys. By using targeted and archival ALMA data in combination with dedicated SED modeling, we retrieve CO and far-infrared (FIR) luminosity as well as M* of SUPER and KASHz host galaxies. We selected non-active galaxies from PHIBBS, ASPECS, and multiple ALMA/NOEMA surveys of submillimeter galaxies in the COSMOS, UDS, and ECDF fields. By matching the samples in redshift, stellar mass, and FIR luminosity, we compared the properties of AGN and non-active galaxies within a Bayesian framework. We find that AGN hosts at given FIR luminosity are on average CO depleted compared to non-active galaxies, thus confirming what was previously found in the SUPER survey. Moreover, the molecular gas fraction distributions of AGN and non-active galaxies are statistically different, with the distribution of AGN being skewed to lower values. Our results indicate that AGN can indeed reduce the total cold molecular gas reservoir of their host galaxies. Lastly, by comparing our results with predictions from three cosmological simulations (TNG, Eagle, and Simba) filtered to match the properties of observed AGN, AGN hosts, and non-active galaxies, we confirm already known discrepancies and highlight new discrepancies between observations and simulations. [ABSTRACT FROM AUTHOR]

Published
2024
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3. SUPER: VIII. Fast and furious at z ∼ 2: Obscured type-2 active nuclei host faster ionised winds than type-1 systems.

Author

Tozzi, G., Cresci, G., Perna, M., Mainieri, V., Mannucci, F., Marconi, A., Kakkad, D., Marasco, A., Brusa, M., Bertola, E., Bischetti, M., Carniani, S., Cicone, C., Circosta, C., Fiore, F., Feruglio, C., Harrison, C. M., Lamperti, I., Netzer, H., and Piconcelli, E.

Subjects
ACTIVE galactic nuclei, ACTIVE galaxies, GALACTIC evolution, ADAPTIVE optics, OPTICAL spectra
Abstract

We present spatially resolved VLT/SINFONI spectroscopy with adaptive optics of type-2 active galactic nuclei (AGN) from the SINFONI Survey for Unveiling the Physics and Effect of Radiative feedback (SUPER), which targeted X-ray bright (L2 − 10 keV ≳ 1042 erg s−1) AGN at cosmic noon (z ∼ 2). Our analysis of the rest-frame optical spectra unveils ionised outflows in all seven examined targets, as traced via [O III]λ5007 line emission, moving at v ≳ 600 km s−1. These outflows are clearly spatially resolved in six objects and extend on 2–4 kpc scales, but they are marginally resolved in the remaining one object. Interestingly, these SUPER type-2 AGN are all heavily obscured sources (NH ≳ 1023 cm−2) and host faster ionised outflows than their type-1 counterparts within the same range of bolometric luminosity (Lbol ∼ 1044.8 − 46.5 erg s−1). SUPER has hence provided observational evidence that the dichotomy of type-1 to type-2 at z ∼ 2 might not be driven simply by projection effects, but might reflect two distinct obscuring life stages of active galaxies, as predicted by evolutionary models. Within this picture, SUPER type-2 AGN might be undergoing the blow-out phase, where the large amount of obscuring material efficiently accelerates large-scale outflows via radiation pressure on dust, eventually unveiling the central active nucleus and signaling the start of the bright, unobscured type-1 AGN phase. Moreover, the velocities of the overall population of ionised outflows detected in SUPER are comparable with the escape speed of their dark matter haloes, and they are in general high enough to reach distances of 30–50 kpc from the centre. These outflows are hence likely to sweep away the gas (at least) out of the baryonic disk and/or to heat the host gas reservoir, thus reducing and possibly quenching star formation. [ABSTRACT FROM AUTHOR]

Published
2024
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4. AGN-driven outflows in clumpy media: multiphase structure and scaling relations.

Author

Ward, S R, Costa, T, Harrison, C M, and Mainieri, V

Subjects
ACTIVE galaxies, GALACTIC evolution, INTERSTELLAR medium, SUPERMASSIVE black holes, ACCRETION disks
Abstract

Small-scale winds driven from accretion discs surrounding active galactic nuclei (AGN) are expected to launch kpc-scale outflows into their host galaxies. However, the ways in which the structure of the interstellar medium (ISM) affects the multiphase content and impact of the outflow remain uncertain. We present a series of numerical experiments featuring a realistic small-scale AGN wind with velocity |$5\times 10^3 \!-\! 10^4\rm {\ km\ s^{-1}}$| interacting with an isolated galaxy disc with a manually controlled clumpy ISM, followed at sub-pc resolution. Our simulations are performed with arepo and probe a wide range of AGN luminosities (⁠|$L_{\rm {AGN}}{=} 10^{43-47}\rm {\ erg\ s^{-1}}$|⁠) and ISM substructures. In homogeneous discs, the AGN wind sweeps up an outflowing, cooling shell, where the emerging cold phase dominates the mass and kinetic energy budgets, reaching a momentum flux |$\dot{p} \approx 7\ L/c$|⁠. However, when the ISM is clumpy, outflow properties are profoundly different. They contain small, long-lived (⁠|$\gtrsim 5\ \rm {Myr}$|⁠), cold (⁠|$T{\lesssim }10^{4.5}{\rm {\ K}}$|⁠) cloudlets entrained in the faster, hot outflow phase, which are only present in the outflow if radiative cooling is included in the simulation. While the cold phase dominates the mass of the outflow, most of the kinetic luminosity is now carried by a tenuous, hot phase with |$T \gtrsim 10^7 \, \rm K$|⁠. While the hot phases reach momentum fluxes |$\dot{p} \approx (1 - 5)\ L/c$|⁠ , energy-driven bubbles couple to the cold phase inefficiently, producing modest momentum fluxes |$\dot{p} \lesssim L/c$| in the fast-outflowing cold gas. These low momentum fluxes could lead to the outflows being misclassified as momentum-driven using common observational diagnostics. We also show predictions for scaling relations between outflow properties and AGN luminosity and discuss the challenges in constraining outflow driving mechanisms and kinetic coupling efficiencies using observed quantities. [ABSTRACT FROM AUTHOR]

Published
2024
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5. Unveiling [C II] clumps in a lensed star-forming galaxy at z ∼ 3.4.

Author

Zanella, A., Iani, E., Dessauges-Zavadsky, M., Richard, J., De Breuck, C., Vernet, J., Kohandel, M., Arrigoni Battaia, F., Bolamperti, A., Calura, F., Chen, C.-C., Devereaux, T., Ferrara, A., Mainieri, V., Pallottini, A., Rodighiero, G., Vallini, L., and Vanzella, E.

Subjects
GALAXIES, COLD gases, MOLECULAR clouds, STAR formation, STARBURSTS, GALACTIC evolution
Abstract

Context. Observations at UV and optical wavelengths have revealed that galaxies at z ∼ 1 − 4 host star-forming regions, dubbed "clumps", which are believed to form due to the fragmentation of gravitationally unstable, gas-rich disks. However, the detection of the parent molecular clouds that give birth to such clumps is still possible only in a minority of galaxies, mostly at z ∼ 1. Aims. We investigated the [C II] and dust morphology of a z ∼ 3.4 lensed galaxy hosting four clumps detected in the UV continuum. We aimed to observe the [C II] emission of individual clumps that, unlike the UV, is not affected by dust extinction, to probe their nature and cold gas content. Methods. We conducted ALMA observations probing scales down to ∼300 pc and detected three [C II] clumps. One (dubbed "NE") coincides with the brightest UV clump, while the other two ("SW" and "C") are not detected in the UV continuum. We do not detect the dust continuum. Results. We converted the [C II] luminosity of individual clumps into molecular gas mass and found Mmol ∼ 108 M⊙. By complementing it with the star formation rate (SFR) estimate from the UV continuum, we estimated the gas depletion time (tdep) of clumps and investigated their location in the Schmidt–Kennicutt plane. While the NE clump has a very short tdep = 0.16 Gyr, which is comparable with high-redshift starbursts, the SW and C clumps instead have longer tdep > 0.65 Gyr and are likely probing the initial phases of star formation. The lack of dust continuum detection is consistent with the blue UV continuum slope estimated for this galaxy (β ∼ −2.5) and it indicates that dust inhomogeneities do not significantly affect the detection of UV clumps in this target. Conclusions. We pushed the observation of the cold gas content of individual clumps up to z ∼ 3.4 and showed that the [C II] line emission is a promising tracer of molecular clouds at high redshift, allowing the detection of clumps with a large range of depletion times. [ABSTRACT FROM AUTHOR]

Published
2024
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6. First results from the JWST Early Release Science Program Q3D: Benchmark Comparison of Optical and Mid-IR Tracers of a Dusty, Ionized Red Quasar Wind at z=0.435

Author

Rupke, D. S. N., Wylezalek, D., Zakamska, N. L., Veilleux, S., Bertemes, C., Ishikawa, Y., Liu, W., Sankar, S., Vayner, A., Lim, H. X. G., McCrory, R., Murphree, G., Whitesell, L., Shen, L., Liu, G., Barrera-Ballesteros, J. K., Chen, H. -W., Diachenko, N., Goulding, A. D., Greene, J. E., Hainline, K. N., Hamann, F., Heckman, T., Johnson, S. D., Lutz, D., Lützgendorf, N., Mainieri, V., Nesvadba, N., Ogle, P., and Sturm, E.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

The [OIII] 5007 A emission line is the most common tracer of warm, ionized outflows in active galactic nuclei across cosmic time. JWST newly allows us to use mid-infrared spectral features at both high spatial and spectral resolution to probe these same winds. Here we present a comparison of ground-based, seeing-limited [OIII] and space-based, diffraction-limited [SIV] 10.51 micron maps of the powerful, kpc-scale outflow in the Type 1 red quasar SDSS J110648.32+480712.3. The JWST data are from the Mid-InfraRed Instrument (MIRI). There is a close match in resolution between the datasets (0."4--0."6), in ionization potential of the O+2 and S+3 ions (35 eV), and in line sensitivity (1e-17 to 2e-17 erg/s/cm2/arcsec2). The [OIII] and [SIV] line shapes match in velocity and linewidth over much of the 20 kpc outflowing nebula, and [SIV] is the brightest line in the rest-frame 3.5--19.5 micron range, demonstrating its usefulness as a mid-IR probe of quasar outflows. [OIII] is nevertheless intriniscally brighter and provides better contrast with the point-source continuum, which is strong in the mid-IR. There is a strong anticorrelation of [OIII]/[SIV] with average velocity, which is consistent with a scenario of differential obscuration between the approaching (blueshifted) and receding (redshifted) sides of the flow. The dust in the wind may also obscure the central quasar, consistent with models that attribute red quasar extinction to dusty winds., Submitted to ApJL

Published
2023

7. Quasar feedback survey: molecular gas affected by central outflows and by ∼10-kpc radio lobes reveal dual feedback effects in 'radio quiet' quasars.

Author

Girdhar, A, Harrison, C M, Mainieri, V, Fernández Aranda, R, Alexander, D M, Arrigoni Battaia, F, Bianchin, M, Calistro Rivera, G, Circosta, C, Costa, T, Edge, A C, Farina, E P, Kakkad, D, Kharb, P, Molyneux, S J, Mukherjee, D, Njeri, A, S., Silpa, Venturi, G, and Ward, S R

Subjects
ACTIVE galactic nuclei, GALAXY clusters, QUASARS, RADIO galaxies, STAR formation, MOLECULAR weights, MOLECULAR structure
Abstract

We present a study of molecular gas, traced via CO (3–2) from Atacama Large Millimeter/submillimeter Array data, of four z < 0.2, 'radio quiet', type 2 quasars (Lbol ∼ 1045.3–1046.2 erg s−1; L |$_{\mathrm{1.4\, GHz}}\sim 10^{23.7}\!-\!10^{24.3}$|   W  Hz−1). Targets were selected to have extended radio lobes (≥ 10 kpc), and compact, moderate-power jets (1–10 kpc; P jet ∼ 1043.2–1043.7 erg s−1). All targets show evidence of central molecular outflows, or injected turbulence, within the gas discs (traced via high-velocity wing components in CO emission-line profiles). The inferred velocities (V out = 250–440 km s−1) and spatial scales (0.6–1.6 kpc), are consistent with those of other samples of luminous low-redshift active galactic nuclei. In two targets, we observe extended molecular gas structures beyond the central discs, containing 9–53  per cent of the total molecular gas mass. These structures tend to be elongated, extending from the core, and wrap-around (or along) the radio lobes. Their properties are similar to the molecular gas filaments observed around radio lobes of, mostly 'radio loud', brightest cluster galaxies. They have the following: projected distances of 5–13 kpc; bulk velocities of 100–340 km s−1; velocity dispersion of 30–130 km s−1; inferred mass outflow rates of 4–20 M⊙ yr−1; and estimated kinetic powers of 1040.3–1041.7 erg s−1. Our observations are consistent with simulations that suggest moderate-power jets can have a direct (but modest) impact on molecular gas on small scales, through direct jet–cloud interactions. Then, on larger scales, jet-cocoons can push gas aside. Both processes could contribute to the long-term regulation of star formation. [ABSTRACT FROM AUTHOR]

Published
2024
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8. The Quasar Feedback Survey: characterizing CO excitation in quasar host galaxies.

Author

Molyneux, S J, Calistro Rivera, G, De Breuck, C, Harrison, C M, Mainieri, V, Lundgren, A, Kakkad, D, Circosta, C, Girdhar, A, Costa, T, Mullaney, J R, Kharb, P, Arrigoni Battaia, F, Farina, E P, Alexander, D M, Ward, S R, Silpa, S, and Smit, R

Subjects
QUASARS, INTERSTELLAR medium, SPECTRAL energy distribution, GALAXIES, IONIZED gases, CARBON monoxide
Abstract

We present a comprehensive study of the molecular gas properties of 17 Type 2 quasars at z < 0.2 from the Quasar Feedback Survey (L |$_{\rm [O~{\small III}]}$| > 1042.1  |$\rm ergs^{-1}$|⁠), selected by their high [O  iii ] luminosities and displaying a large diversity of radio jet properties, but dominated by LIRG-like galaxies. With these data, we are able to investigate the impact of AGN and AGN feedback mechanisms on the global molecular interstellar medium. Using Atacama Pathfinder EXperiment and ALMA ACA observations, we measure the total molecular gas content using the CO(1-0) emission and homogeneously sample the carbon monoxide (CO) spectral line energy distributions, observing CO transitions (J up  = 1, 2, 3, 6, 7). We observe high r 21 ratios (r 21  =  L 'CO(2-1)/ L 'CO(1-0)) with a median r 21  = 1.06, similar to local (U)LIRGs (with r 21 ∼ 1) and higher than normal star-forming galaxies (with r 21 ∼ 0.65). Despite the high r 21 values, for the seven targets with the required data, we find low excitation in CO(6-5) & CO(7-6) (r 61 and r 62 < 0.6 in all but one target), unlike high-redshift quasars in the literature, which are far more luminous and show higher line ratios. The ionized gas traced by [O  iii ] exhibits systematically higher velocities than the molecular gas traced by CO. We conclude that any effects of quasar feedback (e.g. via outflows and radio jets) do not have a significant instantaneous impact on the global molecular gas content and excitation and we suggest that it only occurs on more localized scales. [ABSTRACT FROM AUTHOR]

Published
2024
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10. The AGNIFS survey: spatially resolved observations of hot molecular and ionized outflows in nearby active galaxies.

Author

Riffel, R A, Storchi-Bergmann, T, Riffel, R, Bianchin, M, Zakamska, N L, Ruschel-Dutra, D, Bentz, M C, Burtscher, L, Crenshaw, D M, Dahmer-Hahn, L G, Dametto, N Z, Davies, R I, Diniz, M R, Fischer, T C, Harrison, C M, Mainieri, V, Revalski, M, Rodriguez-Ardila, A, Rosario, D J, and Schönell, A J

Subjects
ACTIVE galactic nuclei, IONIZED gases, SEYFERT galaxies, SPATIAL resolution
Abstract

We present the hot molecular and warm ionized gas kinematics for 33 nearby (0.001 ≲ z ≲ 0.056) X-ray selected active galaxies using the H |$_2\, 2.1218\, \mu$| m and Br γ emission lines observed in the K band with the Gemini near-infrared integral field spectrograph. The observations cover the inner 0.04–2 kpc of each active galactic nucleus at spatial resolutions of 4–250 pc with a velocity resolution of σinst ≈ 20  |${\rm km\, s^{-1}}$|⁠. We find that 31 objects (94 per cent) present a kinematically disturbed region (KDR) seen in ionized gas, while such regions are observed in hot molecular gas for 25 galaxies (76 per cent). We interpret the KDR as being due to outflows with masses of 102–107 and 100–104 M⊙ for the ionized and hot molecular gas, respectively. The ranges of mass-outflow rates (⁠|$\dot{M}_{\rm out}$|⁠) and kinetic power (⁠|$\dot{E}_{\rm K}$|⁠) of the outflows are 10−3–101 M⊙ yr−1 and ∼1037–1043 erg s−1 for the ionized gas outflows, and 10−5–10−2 M⊙ yr−1 and 1035–1039 erg s−1 for the hot molecular gas outflows. The median coupling efficiency in our sample is |$\dot{E}_{\mathrm{K}}/L_{\rm bol}\approx 1.8\times 10^{-3}$| and the estimated momentum fluxes of the outflows suggest they are produced by radiation-pressure in low-density environment, with possible contribution from shocks. [ABSTRACT FROM AUTHOR]

Published
2023
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12. SUPER VII. morphology and kinematics of H α emission in AGN host galaxies at cosmic noon using SINFONI.

Author

Kakkad, D, Mainieri, V, Vietri, G, Lamperti, I, Carniani, S, Cresci, G, Harrison, C, Marconi, A, Bischetti, M, Cicone, C, Circosta, C, Husemann, B, Man, A, Mannucci, F, Netzer, H, Padovani, P, Perna, M, Puglisi, A, Scholtz, J, and Tozzi, G

Subjects
*SEYFERT galaxies, *GALAXIES, *STAR formation, *ADAPTIVE optics, *GALAXY formation, *KINEMATICS
Abstract

We present spatially resolved H α properties of 21 type 1 AGN host galaxies at z ∼ 2 derived from the SUPER survey. These targets were observed with the adaptive optics capabilities of the SINFONI spectrograph, a near-infrared integral field spectrograph, that provided a median spatial resolution of 0.3 arcsec (∼2 kpc). We model the H α emission line profile in each pixel to investigate whether it traces gas in the narrow line region or if it is associated with star formation. To do this, we first investigate the presence of resolved H α emission after subtracting the AGN PSF. We find extended H α emission in 16 out of the 21 type 1 AGN host galaxies (76 per cent). Based on the BPT diagnostics, optical line flux ratios and line widths (FWHM), we show that the H α emission in five galaxies is ionized by the AGN (30 per cent), in four galaxies by star formation (25 per cent) and for the rest (45 per cent), the ionization source is unconstrained. Two galaxies show extended H α FWHM >600 km s−1, which is interpreted as a part of an AGN-driven outflow. Morphological and kinematic maps of H α emission in targets with sufficient signal-to-noise ratio suggest the presence of rotationally supported discs in six galaxies and possible presence of companions in four galaxies. In two galaxies, we find an anticorrelation between the locations of extended H α emission and [O  iii ]-based ionized outflows, indicating possible negative feedback at play. However, in the majority of galaxies, we do not find evidence of outflows impacting H α-based star formation. [ABSTRACT FROM AUTHOR]

Published
2023
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13. The WISSH quasars project: XI. The mean spectral energy distribution and bolometric corrections of the most luminous quasars.

Author

Saccheo, I., Bongiorno, A., Piconcelli, E., Testa, V., Bischetti, M., Bisogni, S., Bruni, G., Cresci, G., Feruglio, C., Fiore, F., Grazian, A., Luminari, A., Lusso, E., Mainieri, V., Maiolino, R., Marconi, A., Ricci, F., Tombesi, F., Travascio, A., and Vietri, G.

Subjects
SPECTRAL energy distribution, STELLAR luminosity function, ACTIVE galactic nuclei, QUASARS, INTERSTELLAR medium
Abstract

Context. Hyperluminous quasi-stellar objects (QSOs) are ideal laboratories to investigate active galactic nucleus (AGN) feedback mechanisms. Their formidable energy release causes powerful winds at all scales, and thus the maximum feedback is expected. Aims. Our aim is to derive the mean spectral energy distribution (SED) of a sample of 85 WISE-SDSS selected hyperluminous (WISSH) quasars. Since the SED provides a direct way to investigate the AGN structure, our goal is to understand if quasars at the bright end of the luminosity function have peculiar properties compared to the bulk of the QSO population. Methods. We collected all the available photometry, from X-rays to the far-infrared (FIR); each WISSH quasar is observed in at least 12 different bands. We then built a mean intrinsic SED after correcting for the dust extinction, absorption and emission lines, and intergalactic medium absorption. We also derived bolometric, IR band, and monochromatic luminosities together with bolometric corrections at λ = 5100 Å and 3 μm. We define a new relation for the 3 μm bolometric correction. Results. We find that the mean SED of hyperluminous WISSH QSOs shows some differences compared to that of less luminous sources (i.e., a lower X-ray emission and a near- and mid-IR excess which can be explained assuming a larger dust contribution. WISSH QSOs have stronger emission from both warm (T ∼ 500 − 600 K) and very hot (T ≥ 1000 K) dust, the latter being responsible for shifting the typical dip of the AGN SED from 1.3 μm to 1.1 μm. We also derived the mean SEDs of two subsamples created based on their spectral features (presence of broad absorption lines and equivalent width of CIV line). We confirm that broad absorption lines (BALs) are X-ray weak and that they have a reddened UV-optical continuum. We also find that BALs tend to have stronger emission from the hot dust component. For sources with a weaker CIV line, our main result is the confirmation of their lower X-ray emission. By populating the LIR vs. z diagram proposed by Symeonidis & Page (MNRAS, 503, 3992), we found that ∼90% of WISSH QSOs with z ≥ 3.5 have their FIR emission dominated by star-forming activity. Conclusions. This analysis suggests that hyperluminous QSOs have a peculiar SED compared to less luminous objects. It is therefore critical to use SED templates constructed exclusively from very bright quasar samples (such as this one) when dealing with particularly luminous sources, such as high-redshift QSOs. [ABSTRACT FROM AUTHOR]

Published
2023
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14. The Chandra Deep Field-South Survey: 7 Ms Source Catalogs

Author

Luo, B, Brandt, W. N, Xue, Y. Q, Lehmer, B, Alexander, D. M, Bauer, F. E, Vito, F, Yang, G, Basu-Zych, A. R, Comastri, A, Gilli, R, Gu, Q.-S, Hornschemeier, A. E, Koekemoer, A, Liu, T, Mainieri, V, Paolillo, M, Ranalli, P, Rosati, P, Schneider, D. P, Shemmer, O, Smail, I, Sun, M, Tozzi, P, Vignali, C, and Wang, J.-X

Subjects
Astrophysics
Abstract

We present X-ray source catalogs for the approx. 7 Ms exposure of the Chandra Deep Field-South (CDF-S), which covers a total area of 484.2 arcmin2. Utilizing WAVDETECT for initial source detection and ACIS Extract for photometric extraction and significance assessment, we create a main source catalog containing 1008 sources that are detected in up to three X-ray bands: 0.5-7.0 keV, 0.5-2.0 keV, and 2-7 keV. A supplementary source catalog is also provided, including 47 lower-significance sources that have bright (Ks < or = 23) near-infrared counterparts. We identify multiwavelength counterparts for 992 (98.4%) of the main-catalog sources, and we collect redshifts for 986 of these sources, including 653 spectroscopic redshifts and 333 photometric redshifts. Based on the X-ray and multiwavelength properties, we identify 711 active galactic nuclei (AGNs) from the main-catalog sources. Compared to the previous approx. 4 Ms CDF-S catalogs, 291 of the main-catalog sources are new detections. We have achieved unprecedented X-ray sensitivity with average flux limits over the central approx. 1 arcmin2 region of 1.9 x 10(exp -17), 6.4 x 10(exp -18), and 2.7 x 10(exp -17) erg/sq cm/s in the three X-ray bands, respectively. We provide cumulative number-count measurements observing, for the first time, that normal galaxies start to dominate the X-ray source population at the faintest 0.5-2.0 keV flux levels. The highest X-ray source density reaches approx. 50,500/sq deg, and 47% +/- 4 of these sources are AGNs (approx. 23,900/sq deg).

Published
2016
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15. Stellar feedback in a clumpy galaxy at z similar to 3.4

Author

Iani, E., Zanella, A., Vernet, J., Richard, J., Gronke, M., Harrison, C. M., Arrigoni-Battaia, F., Rodighiero, G., Burkert, A., Behrendt, M., Chen, Chian-Chou, Emsellem, E., Fensch, J., Hibon, P., Hilker, M., Le Floc'h, E., Mainieri, V., Swinbank, A. M., Valentino, F., Vanzella, E., and Zwaan, M. A.

Subjects
ISM [galaxies], ULTRA DEEP FIELD, STAR-FORMING CLUMPS, Astrophysics::Cosmology and Extragalactic Astrophysics, irregular [galaxies], GIANT CLUMPS, GRAVITATIONALLY LENSED GALAXIES, MOLECULAR GAS FRACTIONS, LY-ALPHA RADIATION, Astrophysics::Solar and Stellar Astrophysics, LYMAN-BREAK GALAXY, INTEGRAL FIELD SPECTROSCOPY, star formation [galaxies], HIGH-REDSHIFT, Astrophysics::Galaxy Astrophysics, evolution [galaxies], high-redshift [galaxies], RESONANCE-LINE RADIATION
Abstract

Giant star-forming regions (clumps) are widespread features of galaxies at z approximate to 1-4. Theory predicts that they can play a crucial role in galaxy evolution, if they survive to stellar feedback for >50 Myr. Numerical simulations show that clumps' survival depends on the stellar feedback recipes that are adopted. Up to date, observational constraints on both clumps' outflows strength and gas removal time-scale are still uncertain. In this context, we study a line-emitting galaxy at redshift z similar or equal to 3.4 lensed by the foreground galaxy cluster Abell 2895. Four compact clumps with sizes less than or similar to 280 pc and representative of the low-mass end of clumps' mass distribution (stellar masses less than or similar to 2 x 10(8) M-circle dot) dominate the galaxy morphology. The clumps are likely forming stars in a starbursting mode and have a young stellar population (similar to 10 Myr). The properties of the Lyman-alpha (Ly alpha) emission and nebular far-ultraviolet absorption lines indicate the presence of ejected material with global outflowing velocities of similar to 200-300 km s(-1). Assuming that the detected outflows are the consequence of star formation feedback, we infer an average mass loading factor (eta) for the clumps of similar to 1.8-2.4 consistent with results obtained from hydrodynamical simulations of clumpy galaxies that assume relatively strong stellar feedback. Assuming no gas inflows (semiclosed box model), the estimates of n suggest that the time-scale over which the outflows expel the molecular gas reservoir (similar or equal to 7 x 10(8 )M(circle dot)) of the four detected low-mass clumps is less than or similar to 50 Myr.

Published
2021
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16. The impact of ionised outflows from z∼2.5 quasars is not through instantaneous in-situ quenching: the evidence from ALMA and VLT/SINFONI

Author

Scholtz, J., Harrison, C.M., Rosario, D.J., Alexander, D.M., Knudsen, K.K., Stanley, F., Chen, C.-C., Kakkad, D., Mainieri, V., and Mullaney, J.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present high-resolution (∼2.4 kpc) ALMA band 7 observations (rest-frame λ ∼ 250μm) of three powerful z∼2.5 quasars (Lbol = 1047.3-1047.5 ergs s−1). These targets have previously been reported as showing evidence for suppressed star formation based on cavities in the narrow Hα emission at the location of outflows traced with [O III] emission. Here we combine the ALMA observations with a re-analysis of the VLT/SINFONI data to map the rest-frame far-infrared emission, Hα emission, and [O III] emission. In all targets we observe high velocity [O III] gas (i.e. W80 ∼ 1000–2000 km s−1) across the whole galaxy. We do not identify any Hα emission that is free from contamination from AGN-related processes; however, based on SED analyses, we show that the ALMA data contains a significant dust-obscured star formation component in two out of the three systems. This dust emission is found to be extended over ≈1.5–5.5 kpc in the nuclear regions, overlaps with the previously reported Hα cavities and is co-spatial with the peak in surface brightness of the [O III] outflows. In summary, within the resolution and sensitivity limits of the data, we do not see any evidence for a instantaneous shut down of in-situ star formation caused directly by the outflows. However, similar to the conclusions of previous studies and based on our measured star formation rates, we do not rule out that the global host galaxy star formation could be suppressed on longer timescales by the cumulative effect of quasar episodes during the growth of these massive black holes.

Published
2021

17. Cosmological simulations predict that AGN preferentially live in gas-rich, star-forming galaxies despite effective feedback.

Author

Ward, S R, Harrison, C M, Costa, T, and Mainieri, V

Subjects
ACTIVE galactic nuclei, GALACTIC evolution, GALAXIES, STAR formation, ACTIVE galaxies, SUPERMASSIVE black holes
Abstract

Negative feedback from active galactic nuclei (AGN) is the leading mechanism for the quenching of massive galaxies in the vast majority of modern galaxy evolution models. However, direct observational evidence that AGN feedback causes quenching on a population scale is lacking. Studies have shown that luminous AGN are preferentially located in gas-rich and star-forming galaxies, an observation that has sometimes been suggested to be in tension with a negative AGN feedback picture. We investigate three of the current cosmological simulations (i llustrisTNG, EAGLE, and SIMBA) along with post-processed models for molecular hydrogen gas masses and perform similar tests to those used by observers. We find that the simulations predict: (i) no strong negative trends between L bol and |$f_{\mathrm{ H}_2}$| or specific star formation rate (sSFR); (ii) both high-luminosity (⁠|$L_{\rm {bol}} \ge 10^{44}\rm {\, erg\, s^{-1}}$|⁠) and high Eddington ratio (λEdd  |$\ge 1{{\ \rm per\ cent}}$|⁠) AGN are preferentially located in galaxies with high molecular gas fractions and sSFR; and (iii) that the gas-depleted and quenched fractions of AGN host galaxies are lower than a control sample of non-active galaxies. These three findings are in qualitative agreement with observational samples at z = 0 and z = 2 and show that such results are not in tension with the presence of strong AGN feedback, which all simulations we employ require to produce realistic massive galaxies. However, we also find quantifiable differences between predictions from the simulations, which could allow us to observationally test the different subgrid feedback models. [ABSTRACT FROM AUTHOR]

Published
2022
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18. Quasar Feedback Survey: revealing the interplay of jets, winds, and emission-line gas in type 2 quasars with radio polarization.

Author

Silpa, S, Kharb, P, Harrison, C M, Girdhar, A, Mukherjee, D, Mainieri, V, and Jarvis, M E

Subjects
QUASARS, IONIZED gases, SPACE telescopes, RADIO galaxies, GASES
Abstract

We present results from a combined radio polarization and emission-line study of five type 2 quasars at z < 0.2 with the Karl G. Jansky Very Large Array (VLA) B-array at 5 GHz and Hubble Space Telescope (HST) [O  iii ] observations. These five sources are known to exhibit close association between radio structures and ionized gas morphology and kinematics. Four sources (J0945+1737, J1000+1242, J1356+1026, and J1430+1339) show polarization in the current data. J1010+1413 is the unpolarized source in our sample. We detect |$0.5{-}1{{\ \rm per\ cent}}$| fractional polarization in the radio cores and a high fractional polarization (⁠|$10{-}30{{\ \rm per\ cent}}$|⁠) in the lobes of these sources. The morphological, spectral, and polarization properties suggest a jet origin for radio emission in J0945+1737, J1000+1242, J1010+1413, and J1430+1339 whereas the current data cannot fully discern the origin of radio emission (jet or wind) in J1356+1026. An anticorrelation between various polarized knots in the radio and [O  iii ] emission is observed in our sources, similar to that observed in some radio-loud AGN in the literature. This suggests that the radio emission is likely to be depolarized by the emission-line gas. By modelling the depolarization effects, we estimate the size of the emission-line gas clouds to be ∼(2.8 ± 1.7) × 10−5 parsec and the amount of thermal material mixed with the synchrotron plasma to be ∼(1.01 ± 0.08) × 106 M⊙ in the lobe of J0945+1737 (which exhibits the most prominent polarization signature in its lobe). The current work demonstrates that the interplay of jets/winds and emission-line gas is most likely responsible for the nature of radio outflows in radio-quiet AGN. [ABSTRACT FROM AUTHOR]

Published
2022
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19. Quasar feedback survey: multiphase outflows, turbulence, and evidence for feedback caused by low power radio jets inclined into the galaxy disc.

Author

Girdhar, A, Harrison, C M, Mainieri, V, Bittner, A, Costa, T, Kharb, P, Mukherjee, D, Arrigoni Battaia, F, Alexander, D M, Calistro Rivera, G, Circosta, C, De Breuck, C, Edge, A C, Farina, E P, Kakkad, D, Lansbury, G B, Molyneux, S J, Mullaney, J R, S, Silpa, and Thomson, A P

Subjects
QUASARS, INTERSTELLAR medium, RADIO jets (Astrophysics), IONIZED gases, TURBULENCE, ELECTRON density, RADIO galaxies
Abstract

We present a study of a luminous, |$z\, =\, 0.15$|⁠ , type-2 quasar (⁠|$L_{[\rm O III]}$|  = 1042.8 erg s−1) from the Quasar Feedback Survey. It is classified as 'radio-quiet' (⁠|$L_{\mathrm{1.4\, GHz}}$|  = 1023.8 W Hz−1); however, radio imaging reveals ∼ 1 kpc low-power radio jets (Pjet = 1044 erg s−1) inclined into the plane of the galaxy disc. We combine MUSE and ALMA observations to map stellar kinematics and ionized and molecular gas properties. The jets are seen to drive galaxy-wide bi-conical turbulent outflows, reaching W 80  = 1000 – 1300 km s−1, in the ionized phase (traced via optical emission lines), which also have increased electron densities compared to the quiescent gas. The turbulent gas is driven perpendicular to the jet axis and is escaping along the galaxy minor axis, reaching 7.5 kpc on both sides. Traced via CO(3–2) emission, the turbulent material in molecular gas phase is one-third as spatially extended and has three times lower velocity-dispersion as compared to ionized gas. The jets are seen to be strongly interacting with the interstellar medium (ISM) through enhanced ionized emission and disturbed/depleted molecular gas at the jet termini. We see further evidence for jet-induced feedback through significantly higher stellar velocity-dispersion aligned, and co-spatial with, the jet axis (⁠|$\lt 5\, ^{\circ }$|⁠). We discuss possible negative and positive feedback scenarios arising due to the interaction of the low-power jets with the ISM in the context of recent jet–ISM interaction simulations, which qualitatively agree with our observations. We discuss how jet-induced feedback could be an important feedback mechanism even in bolometrically luminous 'radio-quiet' quasars. [ABSTRACT FROM AUTHOR]

Published
2022
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20. Obscured AGN at 1.5 < z < 3.0 from the zCOSMOS-deep Survey

Author

Mignoli, M., Feltre, A., Bongiorno, A., Calura, F., Gilli, R., Vignali, C., Zamorani, G., Lilly, S. J., Le Fèvre, O., Bardelli, S., Bolzonella, M., Bordoloi, R., Le Brun, V., Caputi, K. I., Cimatti, A., Diener, C., Garilli, B., Koekemoer, A. M., Maier, C., Mainieri, V., Peng, Y., Pérez Montero, E., Silverman, J. D., Zucca, E., Mignoli, M., Feltre, A., Bongiorno, A., Calura, F., Gilli, R., Vignali, C., Zamorani, G., Lilly, S. J., Le Fèvre, O., Bardelli, S., Bolzonella, M., Bordoloi, R., Le Brun, V., Caputi, K. I., Cimatti, A., Diener, C., Garilli, B., Koekemoer, A. M., Maier, C., Mainieri, V., Peng, Y., Pérez Montero, E., Silverman, J. D., and Zucca, E.

Subjects
galaxies: active, line: formation, galaxies: evolution, galaxies: fundamental parameter, quasars: emission line, X-rays: galaxie
Abstract

Context. The physics and demographics of high-redshift obscured active galactic nuclei (AGN) is still scarcely investigated. New samples of such objects, selected with different techniques, can provide useful insights into their physical properties.Aims. With the goal to determine the properties of the gas in the emitting region of type 2 AGN, in particular, the gas metal content, we exploit predictions from photoionization models, including new parameterizations for the distance of gas distribution from the central source and internal microturbulence in the emitting clouds, to interpret rest-frame UV spectral data.Methods. We selected a sample of 90 obscured (type 2) AGN with 1.45

Published
2019

21. Gemini NIFS survey of feeding and feedback in nearby active galaxies – V. Molecular and ionized gas kinematics.

Author

Bianchin, M, Riffel, R A, Storchi-Bergmann, T, Riffel, R, Ruschel-Dutra, D, Harrison, C M, Dahmer-Hahn, L G, Mainieri, V, Schönell, A J, and Dametto, N Z

Subjects
IONIZED gases, ACTIVE galaxies, ROTATION of galaxies, ACTIVE galactic nuclei, KINEMATICS
Abstract

We study the gas distribution and kinematics of the inner kpc of six moderately luminous (43.43 ≤ log  L bol ≤ 44.83) nearby (0.004 ≤ z ≤ 0.014) Seyfert galaxies observed with the Near-infrared Integral Field Spectrograph (NIFS) in the J (⁠|$1.25\,\mu$| m) and K (⁠|$2.2\,\mu$| m) bands. We analyse the most intense emission lines detected on these spectral wavebands: [Fe  ii ]  |$1.2570\, \mu$| m and Paβ, which trace the ionized gas in the partially and fully ionized regions, and |$\mathrm{ H}_2 \ 2.1218\, \mu$| m, which traces the hot (∼2000 K) molecular gas. The dominant kinematic component is rotation in the disc of the galaxies, except for the ionized gas in NGC 5899 that shows only weak signatures of a disc component. We find ionized gas outflow in four galaxies, while signatures of H2 outflows are seen in three galaxies. The ionized gas outflows display velocities of a few hundred km s−1, and their mass outflow rates are in the range 0.005–12.49 M⊙ yr−1. Their kinetic powers correspond to 0.005–0.7 per cent of the active galactic nuclei (AGN) bolometric luminosities. Besides rotation and outflows signatures in some cases, the H2 kinematics also reveals inflows in three galaxies. The inflow velocities are 50–80 km s−1 and the mass inflow rates are in the range 1–9 × 10−4 M⊙ yr−1 for hot molecular gas. These inflows might be only the hot skin of the total inflowing gas, which is expected to be dominated by colder gas. The mass inflow rates are lower than the current accretion rates to the AGN, and the ionized outflows are apparently disturbing the gas in the inner kpc. [ABSTRACT FROM AUTHOR]

Published
2022
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22. 4MOST: Project overview and information for the First Call for Proposals

Author

de Jong, R. S., Agertz, O., Berbel, A. A., Aird, J., Alexander, D. A., Amarsi, A., Anders, F., Andrae, R., Ansarinejad, B., Ansorge, W., Antilogus, P., Anwand -Heerwart, H., Arentsen, A., Arnadottir, A., Asplund, M., Auger, M., Azais, N., Baade, D., Baker, G., Baker, S., Balbinot, E., Baldry, I. K., Banerji, M., Barden, S., Barklem, P., Barthélémy-Mazot, E., Battistini, C., Bauer, S., Bell, C. P. M., Bellido-Tirado, O., Bellstedt, S., Belokurov, V., Bensby, T., Bergemann, M., Bestenlehner, J. M., Bielby, R., Bilicki, M., Blake, C., Bland-Hawthorn, J., Boeche, C., Boland, W., Boller, T., Bongard, S., Bongiorno, A., Bonifacio, P., Boudon, D., Brooks, D., Brown, M. J. I., Brown, R., Brüggen, M., Brynnel, J., Brzeski, J., Buchert, T., Buschkamp, P., Caffau, E., Caillier, P., Carrick, J., Casagrande, L., Case, S., Casey, A., Cesarini, I., Cescutti, G., Chapuis, D., Chiappini, C., Childress, M., Christlieb, N., Church, R., Cioni, M. -RL., Cluver, M., Colless, M., Collett, T., Comparat, J., Cooper, A., Couch, W., Courbin, F., Croom, S., Croton, D., Daguisé, E., Dalton, G., Davies, L. J. M., Davis, T., de Laverny, P., Deason, A., Dionies, F., Disseau, K., Doel, P., Döscher, D., Driver, S. P., Dwelly, T., Eckert, D., Edge, A., Edvardsson, B., Youssoufi, D. E., Elhaddad, A., Enke, H., Erfanianfar, G., Farrell, T., Fechner, T., Feiz, C., Feltzing, S., Ferreras, I., Feuerstein, D., Feuillet, D., Finoguenov, A., Ford, D., Fotopoulou, S., Fouesneau, M., Frenk, C., Frey, S., Gaessler, W., Geier, S., Fusillo, N. G., Gerhard, O., Giannantonio, T., Giannone, D., Gibson, B., Gillingham, P., González-Fernández, C., Gonzalez-Solares, E., Gottloeber, S., Gould, A., Grebel, E. K., Gueguen, A., Guiglion, G., Haehnelt, M., Hahn, T., Hansen, C. J., Hartman, Henrik, Hauptner, K., Hawkins, K., Haynes, D., Haynes, R., Heiter, U., Helmi, A., Aguayo, C. H., Hewett, P., Hinton, S., Hobbs, D., Hoenig, S., Hofman, D., Hook, I., Hopgood, J., Hopkins, A., Hourihane, A., Howes, L., Howlett, C., Huet, T., Irwin, M., Iwert, O., Jablonka, P., Jahn, T., Jahnke, K., Jarno, A., Jin, S., Jofre, P., Johl, D., Jones, D., Jönsson, H., Jordan, C., Karovicova, I., Khalatyan, A., Kelz, A., Kennicutt, R., King, D., Kitaura, F., Klar, J., Klauser, U., Kneib, J. -P, Koch, A., Koposov, S., Kordopatis, G., Korn, A., Kosmalski, J., Kotak, R., Kovalev, M., Kreckel, K., Kripak, Y., Krumpe, M., Kuijken, K., Kunder, A., Kushniruk, I., Lam, M. I., Lamer, G., Laurent, F., Lawrence, J., Lehmitz, M., Lemasle, B., Lewis, J., Li, B., Lidman, C., Lind, K., Liske, J., Lizon, J. -L, Loveday, J., Ludwig, H. -G, McDermid, R. M., Maguire, K., Mainieri, V., Mali, S., Mandel, H., Mandel, K., Mannering, L., Martell, S., Martinez Delgado, D., Matijevic, G., McGregor, H., McMahon, R., McMillan, P., Mena, O., Merloni, A., Meyer, M. J., Michel, C., Micheva, G., Migniau, J. -E, Minchev, I., Monari, G., Muller, R., Murphy, D., Muthukrishna, D., Nandra, K., Navarro, R., Ness, M., Nichani, V., Nichol, R., Nicklas, H., Niederhofer, F., Norberg, P., Obreschkow, D., Oliver, S., Owers, M., Pai, N., Pankratow, S., Parkinson, D., Paschke, J., Paterson, R., Pecontal, A., Parry, I., Phillips, D., Pillepich, A., Pinard, L., Pirard, J., Piskunov, N., Plank, V., Plüschke, D., Pons, E., Popesso, P., Power, C., Pragt, J., Pramskiy, A., Pryer, D., Quattri, M., Queiroz, A. B. d. A., Quirrenbach, A., Rahurkar, S., Raichoor, A., Ramstedt, S., Rau, A., Recio-Blanco, A., Reiss, R., Renaud, F., Revaz, Y., Rhode, P., Richard, J., Richter, A. D., Rix, H. -W, Robotham, A. S. G., Roelfsema, R., Romaniello, M., Rosario, D., Rothmaier, F., Roukema, B., Ruchti, G., Rupprecht, G., Rybizki, J., Ryde, N., Saar, A., Sadler, E., Sahlén, M., Salvato, M., Sassolas, B., Saunders, W., Saviauk, A., Sbordone, L., Schmidt, T., Schnurr, O., Scholz, R. -D, Schwope, A., Seifert, W., Shanks, T., Sheinis, A., Sivov, T., Skúladóttir, Á., Smartt, S., Smedley, S., Smith, G., Smith, R., Sorce, J., Spitler, L., Starkenburg, E., Steinmetz, M., Stilz, I., Storm, J., Sullivan, M., Sutherland, W., Swann, E., Tamone, A., Taylor, E. N., Teillon, J., Tempel, E., ter Horst, R., Thi, W. -F, Tolstoy, E., Trager, S., Traven, G., Tremblay, P. -E, Tresse, L., Valentini, M., van de Weygaert, R., van den Ancker, M., Veljanoski, J., Venkatesan, S., Wagner, L., Wagner, K., Walcher, C. J., Waller, L., Walton, N., Wang, L., Winkler, R., Wisotzki, L., Worley, C. C., Worseck, G., Xiang, M., Xu, W., Yong, D., Zhao, C., Zheng, J., Zscheyge, F., Zucker, D., Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astronomi, astrofysik och kosmologi, Astronomy, Astrophysics and Cosmology, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, QB
Abstract

We introduce the 4-metre Multi-Object Spectroscopic Telescope (4MOST), a new high-multiplex, wide-field spectroscopic survey facility under development for the four-metre-class Visible and Infrared Survey Telescope for Astronomy (VISTA) at Paranal. Its key specifications are: a large field of view (FoV) of 4.2 square degrees and a high multiplex capability, with 1624 fibres feeding two low-resolution spectrographs ($R = \lambda/\Delta\lambda \sim 6500$), and 812 fibres transferring light to the high-resolution spectrograph ($R \sim 20\,000$). After a description of the instrument and its expected performance, a short overview is given of its operational scheme and planned 4MOST Consortium science; these aspects are covered in more detail in other articles in this edition of The Messenger. Finally, the processes, schedules, and policies concerning the selection of ESO Community Surveys are presented, commencing with a singular opportunity to submit Letters of Intent for Public Surveys during the first five years of 4MOST operations., Comment: Part of the 4MOST issue of The Messenger, published in preparation of 4MOST Community Workshop, see http://www.eso.org/sci/meetings/2019/4MOST.html

Published
2019
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23. Tracing the Mass-Dependent Star Formation History of Late-Type Galaxies using X-ray Emission: Results from the CHANDRA Deep Fields

Author

Lehmer, B.D, Brandt, W.N, Schneider, D.P, Steffen, A.T, Alexander, D.M, Bell, E.F, Hornschemeier, A.E, McIntosh, D.H, Bauer, F.E, Gilli, R, Mainieri, V, Silverman, J.D, Tozzi, P, and Wolf, C

Subjects
Astronomy
Abstract

We report on the X-ray evolution over the last approx.9 Gyr of cosmic history (i.e., since z = 1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S. respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies. which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of approx. 5-10) in the X-ray-to-optical mean luminosity ratio (L(sub x)/L(sub B)) and the X-ray-to-stellar-mass mean ratio (L(sub x)/M(sub *)) for galaxy populations selected by L(sub B) and M(sub *), respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L(sub x)/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR = 1-100 Solar Mass/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star-formation activity out to z approx. 1.4. We find that the star-formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z = 0.2-1, which is consistent with previous studies of how star-formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z approx. 3 and estimate that L(sub x)/L(sub B) at z approx. 3 is similar to its value at z = 1.4.

Published
2008

25. The impact of ionized outflows from z ∼ 2.5 quasars is not through instantaneous in situ quenching: the evidence from ALMA and VLT/SINFONI.

Author

Scholtz, J, Harrison, C M, Rosario, D J, Alexander, D M, Knudsen, K K, Stanley, F, Chen, Chian-Chou, Kakkad, D, Mainieri, V, and Mullaney, J

Subjects
QUASARS, BLACK holes, STAR formation, GALAXY formation, GALACTIC evolution, ACTIVE galaxies, EVIDENCE
Abstract

We present high-resolution (∼2.4 kpc) ALMA band 7 observations (rest-frame λ ∼ 250  |$\mu$| m) of three powerful z  ∼ 2.5 quasars (L bol = 1047.3–1047.5 erg s−1). These targets have previously been reported as showing evidence for suppressed star formation based on cavities in the narrow H α emission at the location of outflows traced with [O  iii ] emission. Here, we combine the ALMA observations with a re-analysis of the VLT/SINFONI data to map the rest-frame far-infrared emission, H α emission, and [O  iii ] emission. In all targets, we observe high velocity [O  iii ] gas (i.e. W80 ∼ 1000–2000 km s−1) across the whole galaxy. We do not identify any H α emission that is free from contamination from AGN-related processes; however, based on SED analyses, we show that the ALMA data contain a significant dust-obscured star formation component in two out of the three systems. This dust emission is found to be extended over ≈1.5–5.5 kpc in the nuclear regions, overlaps with the previously reported H α cavities and is co-spatial with the peak in surface brightness of the [O  iii ] outflows. In summary, within the resolution and sensitivity limits of the data, we do not see any evidence for a instantaneous shut down of in situ star formation caused directly by the outflows. However, similar to the conclusions of previous studies and based on our measured star formation rates, we do not rule out that the global host galaxy star formation could be suppressed on longer time-scales by the cumulative effect of quasar episodes during the growth of these massive black holes. [ABSTRACT FROM AUTHOR]

Published
2021
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26. The quasar feedback survey: discovering hidden Radio-AGN and their connection to the host galaxy ionized gas.

Author

Jarvis, M E, Harrison, C M, Mainieri, V, Alexander, D M, Arrigoni Battaia, F, Calistro Rivera, G, Circosta, C, Costa, T, De Breuck, C, Edge, A C, Girdhar, A, Kakkad, D, Kharb, P, Lansbury, G B, Molyneux, S J, Mukherjee, D, Mullaney, J R, Farina, E P, S, Silpa, and Thomson, A P

Subjects
IONIZED gases, GALAXIES, BRIGHTNESS temperature, RADIO galaxies, BORED piles, QUASARS, SEYFERT galaxies
Abstract

We present the first results from the Quasar Feedback Survey, a sample of 42 z < 0.2, [O  iii ] luminous AGNs (L [O III] > 1042.1 ergs s−1) with moderate radio luminosities (i.e. L 1.4GHz > 1023.4 W Hz−1; median L 1.4GHz = 5.9 × 1023 W Hz−1). Using high spatial resolution (∼0.3–1 arcsec), 1.5–6 GHz radio images from the Very Large Array, we find that 67 per cent of the sample have spatially extended radio features on ∼1–60 kpc scales. The radio sizes and morphologies suggest that these may be lower radio luminosity versions of compact, radio-loud AGNs. By combining the radio-to-infrared excess parameter, spectral index, radio morphology, and brightness temperature, we find radio emission in at least 57 per cent of the sample that is associated with AGN-related processes (e.g. jets, quasar-driven winds, or coronal emission). This is despite only 9.5–21 per cent being classified as radio-loud using traditional criteria. The origin of the radio emission in the remainder of the sample is unclear. We find that both the established anticorrelation between radio size and the width of the [O    iii ] line, and the known trend for the most [O  iii ] luminous AGNs to be associated with spatially extended radio emission, also hold for our sample of moderate radio luminosity quasars. These observations add to the growing evidence of a connection between the radio emission and ionized gas in quasar host galaxies. This work lays the foundation for deeper investigations into the drivers and impact of feedback in this unique sample. [ABSTRACT FROM AUTHOR]

Published
2021
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27. The zCOSMOS survey

Author

Zucca E., Bardelli S., Bolzonella M., Zamorani G., Ilbert O., Pozzetti L., Mignoli M., Kova, #269, Lilly S., Tresse L., Tasca L., Cassata P., Halliday C., Vergani D., Caputi K., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Coppa G., de La Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Pellò R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Abbas U., Bottini D., Cappi A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Meme, P., Meneux B., Oesch P., Porciani C., Scaramella R., Arnouts S., Aussel H., Capak P., Kartaltepe J., Salvato M., Sanders D., Scoville N., Taniguchi Y., Thompson D., CUCCIATI, OLGA, CIMATTI, ANDREA, MORESCO, MICHELE ENNIO MARIA, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF- Milano, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Tokai University, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Materials & Process technology, Boeing Company [Chicago], California Institute of Technology (CALTECH), Sea Mammal Research Unit, St Andrews, Astronomy, Zucca E., Bardelli S., Bolzonella M., Zamorani G., Ilbert O., Pozzetti L., Mignoli M., Kova&#269, K., Lilly S., Tresse L., Tasca L., Cassata P., Halliday C., Vergani D., Caputi K., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Coppa G., Cucciati O., de La Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Pellò R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Abbas U., Bottini D., Cappi A., Cimatti A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Meme, P., Meneux B., Moresco M., Oesch P., Porciani C., Scaramella R., Arnouts S., Aussel H., Capak P., Kartaltepe J., Salvato M., Sanders D., Scoville N., Taniguchi Y., Thompson D., Università di Bologna, Dipartimento di Astronomia, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Normalization (statistics), Cosmology and Nongalactic Astrophysics (astro-ph.CO), High density, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], MORPHOLOGICAL CLASSIFICATION, 1ST EPOCH DATA, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Density field, FIELD, 10. No inequality, 010303 astronomy & astrophysics, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, galaxies: statistics, Luminosity function (astronomy), Physics, REDSHIFT SURVEY, LEGACY SURVEY, 010308 nuclear & particles physics, Galaxies: evolution, Galaxies: luminosity function, mass function, Galaxies: statistics, Astronomy and Astrophysics, Space and Planetary Science, VLT DEEP SURVEY, B band, Galaxy, galaxies: luminosity function, mass function, COLOR-DENSITY RELATION, galaxies: luminosity function, mass function, DIGITAL SKY SURVEY, galaxies: evolution, Cosmic time, SURVEY COSMOS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(Abridged) We studied the evolution in the B band luminosity function to z~1 in the zCOSMOS 10k sample, for which both accurate galaxy classifications and a detailed description of the local density field are available. The global LF exhibits a brightening of ~0.7 mag in M* from z~0.2 to z~0.9. At low z, late types dominate at faint magnitudes, while the bright end is populated mainly by early types. At higher z, late-type galaxies evolve significantly and, at z~1, the contribution from the various types to the bright end of the LF is comparable. The evolution for early types is in both luminosity and normalization. A similar behaviour is exhibited by late types, but with an opposite trend for the normalization. Studying the role of the environment, we find that the global LF of galaxies in overdense regions has always a brighter M* and a flatter slope. In low density environments, the main contribution to the LF is from blue galaxies, while for high density environments there is an important contribution from red galaxies to the bright end. The differences between the global LF in the two environments are not due to only a difference in the relative numbers of red and blue galaxies, but also to their relative luminosity distributions: the value of M* for both types in underdense regions is always fainter than in overdense environments. The "specular" evolution of late- and early-type galaxies is consistent with a scenario where a part of blue galaxies is transformed in red galaxies with increasing cosmic time, without significant changes in the fraction of intermediate-type galaxies. The bulk of this tranformation in overdense regions probably happened before z~1, while it is still ongoing at lower z in underdense environments., Comment: 18 pages, 10 figures, A&A in press

Published
2009
Full Text
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28. XIPE: the x-ray imaging polarimetry explorer

Author

Soffitta, P., Bellazzini, R., Bozzo, E., Burwitz, V., Castro Tirado, A. J., Costa, E., Courvoisier, T., Feng, H., Gburek, S., Goosmann, R., Karas, V., Boettcher, M., Bogdanov, S., Bombaci, I., Bonino, R., Braga, J., Brandt, W., Brez, A., Bucciantini, N., Burderi, L., Caiazzo, I., Matt, G., Campana, R., Campana, S., Capitanio, F., Cappi, M., Cardillo, M., Casella, P., Catmabacak, O., Cenko, B., Cerda Duran, P., Cerruti, C., Muleri, F., Chaty, S., Chauvin, M., Chen, Y., Chenevez, J., Chernyakova, M., Cheung Teddy, C. C., Christodoulou, D., Connell, P., Corbet, R., Coti Zelati, F., Nandra, K., Covino, S., Cui, W., Cusumano, G., D'Ai, A., D'Ammando, F., Dadina, M., Dai, Z., De Rosa, A., De Ruvo, L., Degenaar, N., Pearce, M., Del Santo, M., Del Zanna, L., Dewangan, G., Di Cosimo, S., Di Lalla, N., Di Persio, G., Di Salvo, T., Dias, T., Done, C., Dovciak, M., Poutanen, J., Doyle, G., Ducci, L., Elsner, R., Enoto, T., Escada, J., Esposito, P., Eyles, C., Fabiani, S., Falanga, M., Falocco, S., Reglero, V., Fan, Y., Fender, R., Feroci, M., Ferrigno, C., Forman, W., Foschini, L., Fragile, C., Fuerst, F., Fujita, Y., Gasent Blesa, J. L., Sabau Maria, D., Gelfand, J., Gendre, B., Ghirlanda, G., Ghisellini, G., Giroletti, M., Goetz, D., Gogus, E., Gomez, J. L., Gonzalez, D., Gonzalez Riestra, R., Santangelo, A., Gotthelf, E., Gou, L., Grandi, P., Grinberg, V., Grise, F., Guidorzi, C., Gurlebeck, N., Guver, T., Haggard, D., Hardcastle, M., Tagliaferri, G., Hartmann, D., Haswell, C., Heger, A., Hernanz, M., Heyl, J., Ho, L., Hoormann, J., Horak, J., Huovelin, J., Huppenkothen, D., Tenzer, C., Iaria, R., Inam Sitki, C., Ingram, A., Israel, G., Izzo, L., Burgess, M., Jackson, M., Ji, L., Jiang, J., Vink, J., Johannsen, T., Jones, C., Jorstad, S., Kajava, J. J. E., Kalamkar, M., Kalemci, E., Kallman, T., Kamble, A., Kislat, F., Kiss, M., Weisskopf, M. C., Klochkov, D., Koerding, E., Kolehmainen, M., Koljonen, K., Komossa, S., Kong, A., Korpela, S., Kowalinski, M., Krawczynski, H., Kreykenbohm, I., Zane, S., Kuss, M., Lai, D., Lan, M., Larsson, J., Laycock, S., Lazzati, D., Leahy, D., Li, H., Li, J., L. X., Li, Agudo, I., Li, T., Li, Z., Linares, M., Lister, M., Liu, H., Lodato, G., Lohfink, A., Longo, F., Luna, G., Lutovinov, A., Antonelli, A., Mahmoodifar, S., Maia, J., Mainieri, V., Maitra, C., Maitra, D., Majczyna, A., Maldera, S., Malyshev, D., Manfreda, A., Manousakis, A., Attina, P., Manuel, R., Margutti, R., Marinucci, A., Markoff, S., Marscher, A., Marshall, H., Massaro, F., Mclaughlin, M., Medina Tanco, G., Mehdipour, M., Baldini, L., Middleton, M., Mignani, R., Mimica, P., Mineo, T., Mingo, B., Miniutti, G., Mirac, S. M., Morlino, G., Motlagh, A. V., Motta, S. E., Bykov, A., Mushtukov, A., Nagataki, S., Nardini, F., Nattila, J., Navarro, G. J., Negri, B., Negro, M., Nenonen, S., Neustroev, V., Nicastro, F., Carpentiero, R., Norton, A., Nucita, A., O'Brien, P., O'Dell, S., Odaka, H., Olmi, B., Omodei, N., Orienti, M., Orlandini, M., Osborne, J., Cavazzuti, E., Pacciani, L., Paliya, V. S., Papadakis, I., Papitto, A., Paragi, Z., Pascal, P., Paul, B., Pavan, L., Pellizzoni, A., Perinati, E., Churazov, E., Pesce Rollins, M., Piconcelli, E., Pili, A. G., Pilia, M., Pohl, M., Ponti, G., Porquet, D., Possenti, A., Postnov, K., Prandoni, I., Del Monte, E., Produit, N., Puehlhofer, G., Ramsey, B., Razzano, M., Rea, N., Reig, P., Reinsch, K., Reiprich, T., Reynolds, M., Risaliti, G., De Martino, D., Roberts, T., Rodriguez, J., Rossi, M. E., Rosswog, S., Rozanska, A., Rubini, A., Rudak, B., Russell, D., Ryde, F., Sabatini, S., Donnarumma, I., Sala, G., Salvati, M., Sasaki, M., Savolainen, T., Saxton, R., Scaringi, S., Schawinski, K., Schulz, N. S., Schwope, A., Severgnini, P., Doroshenko, V., Sharon, M., Shaw, A., Shearer, A., Shesheng, X., Shih, I. C., Silva, K., Silva, R., Silver, E., Smale, A., Spada, F., Evangelista, Y., Spandre, G., Stamerra, A., Stappers, B., Starrfield, S., Stawarz, L., Stergioulas, N., Stevens, A., Stiele, H., Suleimanov, V., Sunyaev, R., Ferreira, I., Slowikowska, A., Tamborra, F., Tavecchio, F., Taverna, Roberto, Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Tong, H., Torok, G., Gallo, E., Torres, D. F., Tortosa, A., Tramacere, A., Trimble, V., Trinchieri, G., Tsygankov, S., Tuerler, M., Turriziani, S., Ursini, F., Uttley, P., Grosso, N., Varniere, P., Vincent, F., Vurgun, E., Wang, C., Wang, Z., Watts, A., Wheeler, J. C., Wiersema, K., Wijnands, R., Wilms, J., Kaaret, P., Wolter, A., Wood, K., Wu, K., Wu, X., Xiangyu, W., Xie, F., Xu, R., Yan, S. P., Yang, J., Yu, W., Kuulkers, E., Yuan, F., Zajczyk, A., Zanetti, D., Zanin, R., Zanni, C., Zappacosta, L., Zdziarski, A. A., Zech, A., Zhang, H., Zhang, S., Laranaga, J., Zhang, W., Zoghbi, A., Latronico, L., Lumb, D. H., Macian, J., Malzac, J., Marin, F., Massaro, E., Minuti, M., Mundell, C., Ness, J. U., Oosterbroek, T., Paltani, S., Pareschi, G., Perna, R., Petrucci, P. O., Pinazo, H. B., Pinchera, M., Rodriguez, J. P., Roncadelli, M., Santovincenzo, A., Sazonov, S., Sgro, C., Spiga, D., Svoboda, J., Theobald, C., Theodorou, T., Turolla, Roberto, Wilhelmi De Ona, E., Winter, B., Akbar, A. M., Allan, H., Aloisio, R., Altamirano, D., Amati, L., Amato, E., Angelakis, E., Arezu, J., Atteia, J. L., Axelsson, M., Bachetti, M., Ballo, L., Balman, S., Bandiera, R., Barcons, X., Basso, S., Baykal, A., Becker, W., Behar, E., Beheshtipour, B., Belmont, R., Berger, E., Bernardini, F., Bianchi, S., Bisnovatyi Kogan, G., Blasi, P., Blay, P., Bodaghee, A., Boer, M., Gravitation and Astroparticle Physics Amsterdam, API (FNWI), den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Soffitta, P., Bellazzini, R., Bozzo, E., Burwitz, V., Castro-Tirado, A. J., Costa, E., Courvoisier, T., Feng, H., Gburek, S., Goosmann, R., Karas, V., Matt, G., Muleri, F., Nandra, K., Pearce, M., Poutanen, J., Reglero, V., Sabau Maria, D., Santangelo, A., Tagliaferri, G., Tenzer, C., Vink, J., Weisskopf, M. C., Zane, S., Agudo, I., Antonelli, A., Attina, P., Baldini, L., Bykov, A., Carpentiero, R., Cavazzuti, E., Churazov, E., Del Monte, E., De Martino, D., Donnarumma, I., Doroshenko, V., Evangelista, Y., Ferreira, I., Gallo, E., Grosso, N., Kaaret, P., Kuulkers, E., Laranaga, J., Latronico, L., Lumb, D. H., Macian, J., Malzac, J., Marin, F., Massaro, E., Minuti, M., Mundell, C., Ness, J. U., Oosterbroek, T., Paltani, S., Pareschi, G., Perna, R., Petrucci, P. -O., Pinazo, H. B., Pinchera, M., Rodriguez, J. P., Roncadelli, M., Santovincenzo, A., Sazonov, S., Sgro, C., Spiga, D., Svoboda, J., Theobald, C., Theodorou, T., Turolla, R., Wilhelmi De Ona, E., Winter, B., Akbar, A. M., Allan, H., Aloisio, R., Altamirano, D., Amati, L., Amato, E., Angelakis, E., Arezu, J., Atteia, J. -L., Axelsson, M., Bachetti, M., Ballo, L., Balman, S., Bandiera, R., Barcons, X., Basso, S., Baykal, A., Becker, W., Behar, E., Beheshtipour, B., Belmont, R., Berger, E., Bernardini, F., Bianchi, S., Bisnovatyi-Kogan, G., Blasi, P., Blay, P., Bodaghee, A., Boer, M., Boettcher, M., Bogdanov, S., Bombaci, I., Bonino, R., Braga, J., Brandt, W., Brez, A., Bucciantini, N., Burderi, L., Caiazzo, I., Campana, R., Campana, S., Capitanio, F., Cappi, M., Cardillo, M., Casella, P., Catmabacak, O., Cenko, B., Cerda-Duran, P., Cerruti, C., Chaty, S., Chauvin, M., Chen, Y., Chenevez, J., Chernyakova, M., Cheung Teddy, C. C., Christodoulou, D., Connell, P., Corbet, R., Coti Zelati, F., Covino, S., Cui, W., Cusumano, G., D'Ai, A., D'Ammando, F., Dadina, M., Dai, Z., De Rosa, A., De Ruvo, L., Degenaar, N., Del Santo, M., Del Zanna, L., Dewangan, G., Di Cosimo, S., Di Lalla, N., Di Persio, G., Di Salvo, T., Dias, T., Done, C., Dovciak, M., Doyle, G., Ducci, L., Elsner, R., Enoto, T., Escada, J., Esposito, P., Eyles, C., Fabiani, S., Falanga, M., Falocco, S., Fan, Y., Fender, R., Feroci, M., Ferrigno, C., Forman, W., Foschini, L., Fragile, C., Fuerst, F., Fujita, Y., Gasent-Blesa, J. L., Gelfand, J., Gendre, B., Ghirlanda, G., Ghisellini, G., Giroletti, M., Goetz, D., Gogus, E., Gomez, J. -L., Gonzalez, D., Gonzalez-Riestra, R., Gotthelf, E., Gou, L., Grandi, P., Grinberg, V., Grise, F., Guidorzi, C., Gurlebeck, N., Guver, T., Haggard, D., Hardcastle, M., Hartmann, D., Haswell, C., Heger, A., Hernanz, M., Heyl, J., Ho, L., Hoormann, J., Horak, J., Huovelin, J., Huppenkothen, D., Iaria, R., Inam Sitki, C., Ingram, A., Israel, G., Izzo, L., Burgess, M., Jackson, M., Ji, L., Jiang, J., Johannsen, T., Jones, C., Jorstad, S., Kajava, J. J. E., Kalamkar, M., Kalemci, E., Kallman, T., Kamble, A., Kislat, F., Kiss, M., Klochkov, D., Koerding, E., Kolehmainen, M., Koljonen, K., Komossa, S., Kong, A., Korpela, S., Kowalinski, M., Krawczynski, H., Kreykenbohm, I., Kuss, M., Lai, D., Lan, M., Larsson, J., Laycock, S., Lazzati, D., Leahy, D., Li, H., Li, J., Li, L. -X., Li, T., Li, Z., Linares, M., Lister, M., Liu, H., Lodato, G., Lohfink, A., Longo, F., Luna, G., Lutovinov, A., Mahmoodifar, S., Maia, J., Mainieri, V., Maitra, C., Maitra, D., Majczyna, A., Maldera, S., Malyshev, D., Manfreda, A., Manousakis, A., Manuel, R., Margutti, R., Marinucci, A., Markoff, S., Marscher, A., Marshall, H., Massaro, F., Mclaughlin, M., Medina-Tanco, G., Mehdipour, M., Middleton, M., Mignani, R., Mimica, P., Mineo, T., Mingo, B., Miniutti, G., Mirac, S. M., Morlino, G., Motlagh, A. V., Motta, S. E., Mushtukov, A., Nagataki, S., Nardini, F., Nattila, J., Navarro, G. J., Negri, B., Negro, M., Nenonen, S., Neustroev, V., Nicastro, F., Norton, A., Nucita, A., O'Brien, P., O'Dell, S., Odaka, H., Olmi, B., Omodei, N., Orienti, M., Orlandini, M., Osborne, J., Pacciani, L., Paliya, V. S., Papadakis, I., Papitto, A., Paragi, Z., Pascal, P., Paul, B., Pavan, L., Pellizzoni, A., Perinati, E., Pesce-Rollins, M., Piconcelli, E., Pili, A. G., Pilia, M., Pohl, M., Ponti, G., Porquet, D., Possenti, A., Postnov, K., Prandoni, I., Produit, N., Puehlhofer, G., Ramsey, B., Razzano, M., Rea, N., Reig, P., Reinsch, K., Reiprich, T., Reynolds, M., Risaliti, G., Roberts, T., Rodriguez, J., Rossi, M. E., Rosswog, S., Rozanska, A., Rubini, A., Rudak, B., Russell, D., Ryde, F., Sabatini, S., Sala, G., Salvati, M., Sasaki, M., Savolainen, T., Saxton, R., Scaringi, S., Schawinski, K., Schulz, N. S., Schwope, A., Severgnini, P., Sharon, M., Shaw, A., Shearer, A., Shesheng, X., Shih, I. -C., Silva, K., Silva, R., Silver, E., Smale, A., Spada, F., Spandre, G., Stamerra, A., Stappers, B., Starrfield, S., Stawarz, L., Stergioulas, N., Stevens, A., Stiele, H., Suleimanov, V., Sunyaev, R., Slowikowska, A., Tamborra, F., Tavecchio, F., Taverna, R., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Tong, H., Torok, G., Torres, D. F., Tortosa, A., Tramacere, A., Trimble, V., Trinchieri, G., Tsygankov, S., Tuerler, M., Turriziani, S., Ursini, F., Uttley, P., Varniere, P., Vincent, F., Vurgun, E., Wang, C., Wang, Z., Watts, A., Wheeler, J. C., Wiersema, K., Wijnands, R., Wilms, J., Wolter, A., Wood, K., Wu, K., Wu, X., Xiangyu, W., Xie, F., Xu, R., Yan, S. -P., Yang, J., Yu, W., Yuan, F., Zajczyk, A., Zanetti, D., Zanin, R., Zanni, C., Zappacosta, L., Zdziarski, A. A., Zech, A., Zhang, H., Zhang, S., Zhang, W., Zoghbi, A., Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Castro-Tirado, A., Weisskopf, M., Lumb, D., Ness, J., Petrucci, P., Pinazo, H., Akbar, A., Atteia, J., Cheung Teddy, C., Gasent-Blesa, J., Gomez, J., Kajava, J., Li, L., Mirac, S., Motlagh, A., Motta, S., Navarro, G., Paliya, V., Pili, A., Rossi, M., Schulz, N., Shih, I., Torres, D., Wheeler, J., Yan, S., and Zdziarski, A.

Subjects
X-ray Astronomy, High-energy astronomy, Polarimetry, X-ray optics, X-ray telescope, Condensed Matter Physic, 01 natural sciences, Observatory, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Spectral resolution, Electrical and Electronic Engineering, 010303 astronomy & astrophysics, Gas Pixel Detector, Physics, X-ray astronomy, ta115, 010308 nuclear & particles physics, Electronic, Optical and Magnetic Material, Applied Mathematics, Vega, Astronomy, Computer Science Applications1707 Computer Vision and Pattern Recognition, Condensed Matter Physics, Computer Science Applications, Applied Mathematic, Electronic, Optical and Magnetic Materials, Computer Vision and Pattern Recognition, X-ray optic
Abstract

XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially- resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X-ray astronomers with 75 % of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.

Published
2016

29. SUPER: II. Spatially resolved ionised gas kinematics and scaling relations in z  ∼  2 AGN host galaxies.

Author

Kakkad, D., Mainieri, V., Vietri, G., Carniani, S., Harrison, C. M., Perna, M., Scholtz, J., Circosta, C., Cresci, G., Husemann, B., Bischetti, M., Feruglio, C., Fiore, F., Marconi, A., Padovani, P., Brusa, M., Cicone, C., Comastri, A., Lanzuisi, G., and Mannucci, F.

Subjects
*KINEMATICS, *GALAXIES, *ACTIVE galactic nuclei, *TRACE gases, *STAR formation, *STATISTICAL sampling
Abstract

Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) aims to trace and characterise ionised gas outflows and their impact on star formation in a statistical sample of X-ray selected active galactic nuclei (AGN) at z ∼ 2. We present the first SINFONI results for a sample of 21 Type 1 AGN spanning a wide range in bolometric luminosity (log Lbol = 45.4–47.9 erg s−1). The main aims of this paper are to determine the extension of the ionised gas, characterise the occurrence of AGN-driven outflows, and link the properties of such outflows with those of the AGN. Methods. We used adaptive optics-assisted SINFONI observations to trace ionised gas in the extended narrow line region using the [O III] λ5007 line. We classified a target as hosting an outflow if its non-parametric velocity of the [O III] line, w80, was larger than 600 km s−1. We studied the presence of extended emission using dedicated point-spread function (PSF) observations, after modelling the PSF from the Balmer lines originating from the broad line region. Results. We detect outflows in all the Type 1 AGN sample based on the w80 value from the integrated spectrum, which is in the range ∼650–2700 km s−1. There is a clear positive correlation between w80 and the AGN bolometric luminosity (> 99% correlation probability), and the black hole mass (98% correlation probability). A comparison of the PSF and the [O III] radial profile shows that the [O III] emission is spatially resolved for ∼35% of the Type 1 sample and the outflows show an extension up to ∼6 kpc. The relation between maximum velocity and the bolometric luminosity is consistent with model predictions for shocks from an AGN-driven outflow. The escape fraction of the outflowing gas increases with the AGN luminosity, although for most galaxies, this fraction is less than 10%. [ABSTRACT FROM AUTHOR]

Published
2020
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30. KASHz: No evidence for ionised outflows instantaneously suppressing star formation in moderate luminosity AGN at z ∼ 1.4–2.6.

Author

Scholtz, J, Harrison, C M, Rosario, D J, Alexander, D M, Chen, C-C, Kakkad, D, Mainieri, V, Tiley, A L, Turner, O, Cirasuolo, M, Sharples, R M, and Stach, S

Subjects
STAR formation, LUMINOSITY, ACTIVE galaxies, EVIDENCE, FIR
Abstract

As part of our KMOS AGN Survey at High-redshift (KASHz), we present spatially resolved VLT/KMOS and VLT/SINFONI spectroscopic data and ALMA 870  μ m continuum imaging of eight z  = 1.4–2.6 moderate AGN (⁠|$L_{\rm 2-10 \, \rm kev}$|  = 1042–1045 ergs s−1). We map [O  iii ], H α and rest-frame FIR emission to search for any spatial anticorrelation between ionised outflows (traced by the [O  iii ] line) and star formation (SF; traced by H α and FIR), that has previously been claimed for some high-z AGN and used as evidence for negative and/or positive AGN feedback. First, we conclude that H α is unreliable to map SF inside our AGN host galaxies based on: (i) SF rates inferred from attenuation-corrected H α can lie below those inferred from FIR; (ii) the FIR continuum is more compact than the H α emission by a factor of ∼2 on average; (iii) in half of our sample, we observe significant spatial offsets between the FIR and H α emission, with an average offset of 1.4 ± 0.6 kpc. Secondly, for the five targets with outflows we find no evidence for a spatial anticorrelation between outflows and SF using either H α or FIR as a tracer. This holds for our re-analysis of a famous z  = 1.6 X-ray AGN ('XID 2028') where positive and negative feedback has been previously claimed. Based on our results, any impact on SF by ionised outflows must be subtle, either occurring on scales below our resolution, or on long time-scales. [ABSTRACT FROM AUTHOR]

Published
2020
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31. A Statistical Relation between the X-ray Spectral Index and Eddington Ratio of Active Galactic Nuclei in Deep Surveys

Author

Brightman, M., Silverman, J. D., Mainieri, V., Schramm, M., Steinhardt, C., Kartaltepe, J., Sanders, D. B., Treister, E., Shemmer, O., Brandt, W. N., Brusa, M., Comastri, A., Ho, L. C., Lanzuisi, G., Lusso, E., Nandra, K., Salvato, M., Zamorani, G., Alexander, D. M., Bongiorno, A., Capak, P., Civano, F., Del, Moro A., Elvis, M., Hasinger, G., Ueda, Y., Matsuoka, K., Nagao, T., Akiyama, M., Doi, Akihiro, M. Brightman, J. D. Silverman, V. Mainieri, Y. Ueda, M. Schramm, K. Matsuoka, T. Nagao, C. Steinhardt, J. Kartaltepe, D. B. Sander, E. Treister, O. Shemmer, W. N. Brandt, M. Brusa, A. Comastri, L. C. Ho, G. Lanzuisi, E. Lusso, K. Nandra, M. Salvato, G. Zamorani, M. Akiyama, D. M. Alexander, A. Bongiorno, P. Capak, F. Civano, A. . Moro, A. Doi, M. Elvi, G. Hasinger, E. S. Laird, D. Master, M. Mignoli, K. Ohta, K. Schawinski, and Y. Taniguchi

Subjects
Accretion, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, galaxies. [X-rays], galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, emission lines [Quasars], accretion, accretion disc, quasars: general, Bolometric correction, Emission spectrum, Accretion discs, Galaxies: Active, Galaxies: Nuclei, Quasars: Emission lines, Quasars: General, X-rays: galaxies, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, Supermassive black hole, Astronomy, general [Quasars], Astronomy and Astrophysics, Quasar, Space and Planetary Science, nuclei [Galaxies], Chandra Deep Field South, Spectral energy distribution, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena, quasars: emission line, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数: 36名, Accepted: 2013-05-22, 資料番号: SA1004651000

Published
2013

32. Ionised outflows in z similar to 2.4 quasar host galaxies

Author

Carniani, S., Marconi, A., Maiolino, R., Balmaverde, B., Brusa, M., Cano Díaz, M., Cicone, C., Comastri, A., Cresci, G., Fiore, F., Feruglio, C., Mainieri, V., Mannucci, F., Nagao, T., Netzer, H., Piconcelli, E., Risaliti, G., Schneider, R., Shemmer, O., LA FRANCA, Fabio, Carniani, S., Marconi, A., Maiolino, R., Balmaverde, B., Brusa, M., Cano Díaz, M., Cicone, C., Comastri, A., Cresci, G., Fiore, F., Feruglio, C., LA FRANCA, Fabio, Mainieri, V., Mannucci, F., Nagao, T., Netzer, H., Piconcelli, E., Risaliti, G., Schneider, R., and Shemmer, O.

Subjects
galaxies: active, galaxies: evolution, quasars: emission lines, techniques: imaging spectroscopy, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Aims. Outflows driven by active galactic nuclei (AGN) are invoked by galaxy evolutionary models to quench star formation and to explain the origin of the relations observed locally between super-massive black holes and their host galaxies. We here aim to detect extended ionised outflows in luminous quasars, where we expect the highest activity both in star formation and in black-hole accretion. Currently, there are only a few studies based on spatially resolved observations of outflows at high redshift, z > 2. Methods. We analysed a sample of six luminous (L > 10(47) erg/s) quasars at z similar to 2.4, observed in H-band using the near-IR integral field spectrometer SINFONI at the VLT. We performed a kinematic analysis of the [OIII] emission line at lambda = 5007 angstrom. Results. We detect fast, spatially extended outflows in five out of six targets. [OIII]lambda 5007 has a complex gas kinematic, with blue-shifted velocities of a few hundreds of km s(-1) and line widths up to 1500 km s(-1). Using the spectroastrometric method, we infer a size of the ionised outflows of up to similar to 2 kpc. The properties of the ionised outflows, mass outflow rate, momentum rate, and kinetic power, are correlated with the AGN luminosity. The increase in outflow rate with increasing AGN luminosity is consistent with the idea that a luminous AGN pushes away the surrounding gas through fast outflows that are driven by radiation pressure, which depends on the emitted luminosity. Conclusions. We derive mass outflow rates of about 6 700 M-circle dot yr(-1) for our sample, which are lower than those observed in molecular outflows. The physical properties of ionised outflows show dependences on AGN luminosity that are similar to those of molecular outflows, but indicate that the mass of ionised gas is lower than that of molecular outflows. Alternatively, this discrepancy between ionised and molecular outflows could be explained with different acceleration mechanisms.

Published
2015

33. VizieR Online Data Catalog: COSMOS photometric redshift catalog (Ilbert+, 2009)

Author

Ilbert, O., Capak, P., Salvato, M., Aussel, H., Mccracken, H. J., Sanders, D. B., Scoville, N., Kartaltepe, J., Arnouts, S., Le Floc H, E., Mobasher, B., Taniguchi, Y., Lamareille, F., Leauthaud, A., Sasaki, S., Thompson, D., Zamojski, M., Zamorani, G., Bardelli, S., Bolzonella, M., Angela Bongiorno, Brusa, M., Caputi, K. I., Carollo, C. M., Contini, T., Cook, R., Coppa, G., Cucciati, O., La Torre, S., Ravel, L., Franzetti, P., Garilli, B., Hasinger, G., Iovino, A., Kampczyk, P., Kneib, J. -P, Knobel, C., Kovac, K., Le Borgne, J. F., Le Brun, V., Fevre, O. L., Lilly, S., Looper, D., Maier, C., Mainieri, V., Mellier, Y., Mignoli, M., Murayama, T., Pello, R., Peng, Y., Perez-Montero, E., Renzini, A., Ricciardelli, E., Schiminovich, D., Scodeggio, M., Shioya, Y., Silverman, J., Surace, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Photometry, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Redshifts, Surveys, Galaxy catalogs
Published
2017

34. Investigating the relationship between AGN activity and stellar mass in zCOSMOS galaxies at 0

Author

Vitale, M, Mignoli, M, Cimatti, A, Lilly, S, Carollo, C, Contini, T, Kneib, J, Fevre, O, Mainieri, V, Renzini, A, Scodeggio, M, Zamorani, G, Bardelli, S, Barnes, L, Bolzonella, M, Bongiorno, A, Bordoloi, R, Bschorr, T, Cappi, A, Caputi, K, Coppa, G, Cucciati, O, Torre, S, Ravel, L, and Franzetti, P

Abstract

We investigate the link between AGN activity, star-formation and stellar mass of the host galaxy at 010.2 threshold. Moreover, the stellar populations of AGN hosts are found to be older with respect to star-forming and composites galaxies. This could be due to the the tendency of AGN to reside in massive hosts. The dependence of the AGN classification on the stellar mass is in agreement with what has been already found in previous studies. It is consistent with, together with the evidence of older stellar populations inhabiting the AGN-like galaxies, the downsizing scenario. In particular, our evidence points to an evolutionary scenario where the AGN-feedback is capable of quenching the star formation in the most massive galaxies. Therefore, the AGN-feedback is the best candidate for initiating the passive evolutionary phase of galaxies.

Published
2016

35. Understanding the shape of the galaxy two-point correlation function at z~1 in the COSMOS field

Author

Torre, S, Guzzo, L, Kovac, K, Porciani, C, Abbas, U, Meneux, B, Carollo, C, Contini, T, Kneib, J, Fevre, O, Lilly, S, Mainieri, V, Renzini, A, Sanders, D, Scodeggio, M, Scoville, N, Zamorani, G, Bardelli, S, Bolzonella, M, Bongiorno, A, Caputi, K, Coppa, G, Cucciati, O, Ravel, L, and Franzetti, P

Abstract

We investigate how the shape of the galaxy two-point correlation function as measured in the zCOSMOS survey depends on local environment, quantified in terms of the density contrast on scales of 5 Mpc/h. We show that the flat shape previously observed at redshifts between z=0.6 and z=1 can be explained by this volume being simply 10% over-abundant in high-density environments, with respect to a Universal density probability distribution function. When galaxies corresponding to the top 10% tail of the distribution are excluded, the measured w_p(r_p) steepens and becomes indistinguishable from LCDM predictions on all scales. This is the same effect recognised by Abbas and Sheth in the SDSS data at z~0 and explained as a natural consequence of halo-environment correlations in a hierarchical scenario. Galaxies living in high-density regions trace dark matter halos with typically higher masses, which are more correlated. If the density probability distribution function of the sample is particularly rich in high-density regions because of the variance introduced by its finite size, this produces a distorted two-point correlation function. We argue that this is the dominant effect responsible for the observed "peculiar" clustering in the COSMOS field.

Published
2016
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36. Proto-groups at 1.8

Author

Diener, C, Lilly, S, Knobel, C, Zamorani, G, Lemson, G, Kampczyk, P, Scoville, N, Carollo, C, Contini, T, Kneib, J, Fevre, O, Mainieri, V, Renzini, A, Scodeggio, M, Bardelli, S, Bolzonella, M, Bongiorno, A, Caputi, K, Cucciati, O, Torre, S, Ravel, L, Franzetti, P, Garilli, B, Iovino, A, and Kovač, K

Abstract

We identify 42 candidate groups lying between 1.8

Published
2016

37. The COSMOS Density Field: A Reconstruction Using Both Weak Lensing and Galaxy Distributions

Author

Amara, A, Lilly, S, Kovac, K, Rhodes, J, Massey, R, Zamorani, G, Carollo, C, Contini, T, Kneib, J, Fevre, O, Mainieri, V, Renzini, A, Scodeggio, M, Bardelli, S, Bolzonella, M, Bongiorno, A, Caputi, K, Cucciati, O, Torre, S, Ravel, L, Franzetti, P, Garilli, B, Iovino, A, Kampczyk, P, and Knobel, C

Abstract

The COSMOS field has been the subject of a wide range of observations, with a number of studies focusing on reconstructing the 3D dark matter density field. Typically, these studies have focused on one given method or tracer. In this paper, we reconstruct the distribution of mass in the COSMOS field out to a redshift z=1 by combining Hubble Space Telescope weak lensing measurements with zCOSMOS spectroscopic measurements of galaxy clustering. The distribution of galaxies traces the distribution of mass with high resolution (particularly in redshift, which is not possible with lensing), and the lensing data empirically calibrates the mass normalisation (bypassing the need for theoretical models). Two steps are needed to convert a galaxy survey into a density field. The first step is to create a smooth field from the galaxy positions, which is a point field. We investigate four possible methods for this: (i) Gaussian smoothing, (ii) convolution with truncated isothermal sphere, (iii) fifth nearest neighbour smoothing and (iv) a muliti-scale entropy method. The second step is to rescale this density field using a bias prescription. We calculate the optimal bias scaling for each method by comparing predictions from the smoothed density field with the measured weak lensing data, on a galaxy-by-galaxy basis. In general, we find scale-independent bias for all the smoothing schemes, to a precision of 10%. For the nearest neighbour smoothing case, we find the bias to be 2.51\pm 0.25. We also find evidence for a strongly evolving bias, increasing by a factor of ~3.5 between redshifts 0

Published
2016
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38. X-ray Groups of Galaxies at 0.5

Author

Tanaka, M, Finoguenov, A, Lilly, S, Bolzonella, M, Carollo, C, Contini, T, Iovino, A, Kneib, J, Lamareille, F, Fevre, O, Mainieri, V, Presotto, V, Renzini, A, Scodeggio, M, Silverman, J, Zamorani, G, Bardelli, S, Bongiorno, A, Caputi, K, Cucciati, O, Torre, S, Ravel, L, Franzetti, P, Garilli, B, and Kampczyk, P

Abstract

We present a photometric and spectroscopic study of galaxies at 0.5

Published
2016

39. XIPE

Author

Soffitta, P., Bellazzini, R., Bozzo, E., Burwitz, V., Castro-Tirado, A. J., Costa, E., Courvoisier, T., Feng, H., Gburek, S., Goosmann, R., Karas, V., Matt, G., Muleri, F., Nandra, K., Pearce, M., Poutanen, J., Reglero, V., Sabau Maria, D., Santangelo, A., Tagliaferri, G., Tenzer, C., Vink, J., Weisskopf, M. C., Zane, S., Agudo, I., Antonelli, A., Attina, P., Baldini, L., Bykov, A., Carpentiero, R., Cavazzuti, E., Churazov, E., Del Monte, E., De Martino, D., Donnarumma, I., Doroshenko, V., Evangelista, Y., Ferreira, I., Gallo, E., Grosso, N., Kaaret, P., Kuulkers, E., Laranaga, J., Latronico, L., Lumb, D. H., Macian, J., Malzac, J., Marin, F., Massaro, E., Minuti, M., Mundell, C., Ness, J. U., Oosterbroek, T., Paltani, S., Pareschi, G., Perna, R., Petrucci, P. O., Pinazo, H. B., Pinchera, M., Rodriguez, J. P., Roncadelli, M., Santovincenzo, A., Sazonov, S., Sgro, C., Spiga, D., Svoboda, J., Theobald, C., Theodorou, T., Turolla, R., Wilhelmi De Ona, E., Winter, B., Akbar, A. M., Allan, H., Aloisio, R., Altamirano, D., Amati, L., Amato, E., Angelakis, E., Arezu, J., Atteia, J. L., Axelsson, M., Bachetti, M., Ballo, L., Balman, S., Bandiera, R., Barcons, X., Basso, S., Baykal, A., Becker, W., Behar, E., Beheshtipour, B., Belmont, R., Berger, E., Bernardini, F., Bianchi, S., Bisnovatyi-Kogan, G., Blasi, P., Blay, P., Bodaghee, A., Boer, M., Boettcher, M., Bogdanov, S., Bombaci, I., Bonino, R., Braga, J., Brandt, W., Brez, A., Bucciantini, N., Burderi, L., Caiazzo, I., Campana, R., Campana, S., Capitanio, F., Cappi, M., Cardillo, M., Casella, P., Catmabacak, O., Cenko, B., Cerda-Duran, P., Cerruti, C., Chaty, S., Chauvin, M., Chen, Y., Chenevez, J., Chernyakova, M., Cheung Teddy, C. C., Christodoulou, D., Connell, P., Corbet, R., Coti Zelati, F., Covino, S., Cui, W., Cusumano, G., D'Ai, A., D'Ammando, F., Dadina, M., Dai, Z., De Rosa, A., De Ruvo, L., Degenaar, N., Del Santo, M., Del Zanna, L., Dewangan, G., Di Cosimo, S., Di Lalla, N., Di Persio, G., Di Salvo, T., Dias, T., Done, C., Dovciak, M., Doyle, G., Ducci, L., Elsner, R., Enoto, T., Escada, J., Esposito, P., Eyles, C., Fabiani, S., Falanga, M., Falocco, S., Fan, Y., Fender, R., Feroci, M., Ferrigno, C., Forman, W., Foschini, L., Fragile, C., Fuerst, F., Fujita, Y., Gasent-Blesa, J. L., Gelfand, J., Gendre, B., Ghirlanda, G., Ghisellini, G., Giroletti, M., Goetz, D., Gogus, E., Gomez, J. L., Gonzalez, D., Gonzalez-Riestra, R., Gotthelf, E., Gou, L., Grandi, P., Grinberg, V., Grise, F., Guidorzi, C., Gurlebeck, N., Guver, T., Haggard, D., Hardcastle, M., Hartmann, D., Haswell, C., Heger, A., Hernanz, M., Heyl, J., Ho, L., Hoormann, J., Horak, J., Huovelin, J., Huppenkothen, D., Iaria, R., Inam Sitki, C., Ingram, A., Israel, G., Izzo, L., Burgess, M., Jackson, M., Ji, L., Jiang, J., Johannsen, T., Jones, C., Jorstad, S., Kajava, J. J E, Kalamkar, M., Kalemci, E., Kallman, T., Kamble, A., Kislat, F., Kiss, M., Klochkov, D., Koerding, E., Kolehmainen, M., Koljonen, K., Komossa, S., Kong, A., Korpela, S., Kowalinski, M., Krawczynski, H., Kreykenbohm, I., Kuss, M., Lai, D., Lan, M., Larsson, J., Laycock, S., Lazzati, D., Leahy, D., Li, H., Li, J., Li, L. X., Li, T., Li, Z., Linares, M., Lister, M., Liu, H., Lodato, G., Lohfink, A., Longo, F., Luna, G., Lutovinov, A., Mahmoodifar, S., Maia, J., Mainieri, V., Maitra, C., Maitra, D., Majczyna, A., Maldera, S., Malyshev, D., Manfreda, A., Manousakis, A., Manuel, R., Margutti, R., Marinucci, A., Markoff, S., Marscher, A., Marshall, H., Massaro, F., McLaughlin, M., Medina-Tanco, G., Mehdipour, M., Middleton, M., Mignani, R., Mimica, P., Mineo, T., Mingo, B., Miniutti, G., Mirac, S. M., Morlino, G., Motlagh, A. V., Motta, S. E., Mushtukov, A., Nagataki, S., Nardini, F., Nattila, J., Navarro, G. J., Negri, B., Negro, M., Nenonen, S., Neustroev, V., Nicastro, F., Norton, A., Nucita, A., O'Brien, P., O'Dell, S., Odaka, H., Olmi, B., Omodei, N., Orienti, M., Orlandini, M., Osborne, J., Pacciani, L., Paliya, V. S., Papadakis, I., Papitto, A., Paragi, Z., Pascal, P., Paul, B., Pavan, L., Pellizzoni, A., Perinati, E., Pesce-Rollins, M., Piconcelli, E., Pili, A. G., Pilia, M., Pohl, Martin, Ponti, G., Porquet, D., Possenti, A., Postnov, K., Prandoni, I., Produit, N., Puehlhofer, G., Ramsey, B., Razzano, M., Rea, N., Reig, P., Reinsch, K., Reiprich, T., Reynolds, M., Risaliti, G., Roberts, T., Rodriguez, J., Rossi, M. E., Rosswog, S., Rozanska, A., Rubini, A., Rudak, B., Russell, D., Ryde, F., Sabatini, S., Sala, G., Salvati, M., Sasaki, M., Savolainen, T., Saxton, R., Scaringi, S., Schawinski, K., Schulz, N. S., Schwope, A., Severgnini, P., Sharon, M., Shaw, A., Shearer, A., Shesheng, X., Shih, I. C., Silva, K., Silva, R., Silver, E., Smale, A., Spada, F., Spandre, G., Stamerra, A., Stappers, B., Starrfield, S., Stawarz, L., Stergioulas, N., Stevens, A., Stiele, H., Suleimanov, V., Sunyaev, R., Slowikowska, A., Tamborra, F., Tavecchio, F., Taverna, R., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Tong, H., Torok, G., Torres, D. F., Tortosa, A., Tramacere, A., Trimble, V., Trinchieri, G., Tsygankov, S., Tuerler, M., Turriziani, S., Ursini, F., Uttley, P., Varniere, P., Vincent, F., Vurgun, E., Wang, C., Wang, Z., Watts, A., Wheeler, J. C., Wiersema, K., Wijnands, R., Wilms, J., Wolter, A., Wood, K., Wu, K., Wu, X., Xiangyu, W., Xie, F., Xu, R., Yan, S. P., Yang, J., Yu, W., Yuan, F., Zajczyk, A., Zanetti, D., Zanin, R., Zanni, C., Zappacosta, L., Zdziarski, A. A., Zech, A., Zhang, H., Zhang, S., Zhang, W., Zoghbi, A., den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Istituto di Astrofisica e Planetologia Spaziali, University of Pisa, University of Geneva, Max Planck Institute for Extraterrestrial Physics, CSIC, Tsinghua University, Polish Academy of Sciences, Université de Strasbourg, Czech Academy of Sciences, Roma Tre University, KTH Royal Institute of Technology, University of Turku, Universidad de Valencia, Instituto Nacional de Tecnica Aeroespacial, University of Tübingen, INAF—Osservatorio Astronomico di Brera, University of Amsterdam, National Aeronautics and Space Administration, University College London, ASI Science Data Center, Ioffe Institute, Agenzia Spaziale Italiana, Max-Planck-Institut für Astrophysik, INAF Osservatorio Astronomico di Capodimonte, European Space Research and Technology Centre, University of Michigan, Ann Arbor, Michigan State University, INFN, Sezione di Torino, IRAP, Università La Sapienza, INFN Pisa, University of Bath, European Space Astronomy Centre, Stony Brook University, Université Grenoble Alpes, Istituto Nazionale di Fisica Nucleare (INFN), Russian Academy of Sciences, University of Padova, Autonomous University of Barcelona, Effat University, Danmarks Tekniske Universitet, Osservatorio Astrofisico Di Arcetri, Florence, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, Max Planck Institute for Radio Astronomy, Buein Zahra Technical University, Osservatorio Astronomico Cagliari, Middle East Technical University, Universidad de Cantabria, Osservatorio Astronomicodi Roma, Technion-Israel Institute of Technology, Washington University St. Louis, Harvard University, New York University Abu Dhabi, Space Research Institute of the Russian Academy of Sciences, Georgia College, Centre National de la Recherche Scientifique (CNRS), North West University, Columbia University, Sapienza University of Rome, Instituto Nacional de Pesquisas Espaciais, Pennsylvania State University, University of Cagliari, University of British Columbia, INAF/IASF Bologna, INAF, Osservatorio Astronomico di Roma, Sabanci University, Université Paris Diderot, Nanjing University, Dublin City University, Naval Research Laboratory, University of Massachusetts Lowell, University of Maryland, Baltimore, Purdue University, INAF-IASF Palermo, University of Palermo, Inter-University Centre for Astronomy and Astrophysics India, Durham University, Armagh Observatory, NASA Goddard Space Flight Center, Universidade de Coimbra, INAF/IASF Milano, International Space Science Institute, University of Naples Federico II, CAS - Purple Mountain Observatory, University of Oxford, College of Charleston, California Institute of Technology, Osaka University, University of the Virgin Islands, European Space Agency - ESA, Chinese Academy of Sciences, Massachusetts Institute of Technology, University of Bremen, Istanbul University, McGill University, University of Hertfordshire, Clemson University, Open University Milton Keynes, Monash University, University of Helsinki, Cardiff University, CAS - Institute of High Energy Physics, Fudan University, Perimeter Institute for Theoretical Physics, Boston University, Radboud University Nijmegen, National Tsing Hua University, Friedrich-Alexander University Erlangen-Nürnberg, Cornell University, Oregon State University, University of Calgary, Kavli Institute for Astronomy and Astrophysics, XiangTan University, Guangxi University, University of Milano, University of Cambridge, Università Degli Studi di Trieste, Universidad de Buenos Aires, European Southern Observatory, Wheaton College, National Centre for Nuclear Research, Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences, New York University, West Virginia University, Universidad Nacional Autónoma de México, SRON Netherlands Institute for Space Research, University of Leicester, Gran Sasso Science Institute, RIKEN, Keele University, Oxford Instruments Analytical Oy, University of Salento, JAXA Institute of Space and Astronautical Science, University of Florence, Kavli Institute for Particle Astrophysics and Cosmology, University of Crete, Joint Institute for VLBI in Europe, Université Paul Sabatier, Raman Research Institute, Lomonosov Moscow State University, Foundation for Research and Technology - Hellas, University of Göttingen, Argelander-Institut für Astronomie, Leiden University, Stockholm University, Polytechnic University of Catalonia, Metsähovi Radio Observatory, Swiss Federal Institute of Technology Zurich, Leibniz Institut für Astrophysik Potsdam, University of Alberta, University of Southampton, National University of Ireland, Galway, Paris Observatory, INAF—Osservatorio Astrofisico di Torino, University of Manchester, Arizona State University, Jagiellonian University in Kraków, Aristotle University of Thessaloniki, University of Zielona Gora, Istituto Universitario di Studi Superiori di Pavia, University of Maryland, College Park, University of California Berkeley, Silesian University in Opava, University of California Irvine, Università di Roma Tor Vergata, Institut national de physique nucléaire et de physique des particules, Université Pierre and Marie Curie, Tongji University, University of Texas at Austin, Peking University, CAS - Shanghai Astronomical Observatory, Technische Universität Darmstadt, Los Alamos National Laboratory, Aalto-yliopisto, and Aalto University

Subjects
X-ray Astronomy, X-ray optics, Polarimetry, Gas Pixel Detector
Abstract

XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially-resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X-ray astronomers with 75 % of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.

Published
2016

40. The Chandra Deep Field South: the 1 Million Second

Author

Rosati, P., Tozzi, P., Giacconi, R., Gilli, R., Hasinger, G., Kewley, L., Mainieri, V., Nonino, M., Colin Norman, Szokoly, G., Wang, J. X., Zirm, A., Bergeron, J., Borgani, S., Gilmozzi, R., Grogin, N., Koekemoer, A., Schreier, E., and Zheng, W.

Subjects
astro-ph, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

We present the main results from our 940 ksec observation of the Chandra Deep Field South (CDFS), using the source catalog described in an accompanying paper (Giacconi et al. 2001). We extend the measurement of source number counts to 5.5e-17 erg/cm^2/s in the soft 0.5-2 keV band and 4.5e-16 erg/cm^2/s in the hard 2-10 keV band. The hard band LogN-LogS shows a significant flattening (slope~=0.6) below ~1e-14 erg/cm^2/s, leaving at most 10-15% of the X-ray background (XRB) to be resolved, the main uncertainty lying in the measurement of the total flux of the XRB. On the other hand, the analysis in the very hard 5-10 keV band reveals a relatively steep LogN-LogS (slope ~=1.3) down to 1e-15 erg/cm^2/s. Together with the evidence of a progressive flattening of the average X-ray spectrum near the flux limit, this indicates that there is still a non negligible population of faint hard sources to be discovered at energies not well probed by Chandra, which possibly contribute to the 30 keV bump in the spectrum of the XRB. We use optical redshifts and identifications, obtained with the VLT, for one quarter of the sample to characterize the combined optical and X-ray properties of the CDFS sample. Different source types are well separated in a parameter space which includes X-ray luminosity, hardness ratio and R-K color. Type II objects, while redder on average than the field population, have colors which are consistent with being hosted by a range of galaxy types. Type II AGN are mostly found at z, Comment: Accepted by The Astrophysical Journal, 24 pages, 8 figures, 1 color jpg plate (fig.1)

Published
2015

41. Extreme emission-line galaxies out to z similar to 1 in zCOSMOS I. Sample and characterization of global properties

Author

Amorin, R., Perez-Montero, F., Contini, T., Vilchez, J. M., Bolzonella, M., Tasca, L. A. M., Lamareille, F., Zamorani, G., Maier, C., Carollo, C. M., Kneib, J. -P., Le Fevre, O., Lilly, S., Mainieri, V., Renzinis, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Kovac, K., Le Borgne, J. -F., Le Brun, V., Mignoli, M., Pello, R., Peng, Y., Presotto, V., Ricciardelli, E., Silverman, J. D., Tanaka, M., Tresse, L., Vergani, D., Zucca, E., and Kapteyn Astronomical Institute

Subjects
ACTIVE GALACTIC NUCLEI, galaxies: irregular galaxies: star formation, ULTRA DEEP FIELD, METAL-POOR GALAXIES, galaxies: fundamental parameters, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, LYMAN BREAK GALAXIES, LY-ALPHA EMITTERS, LUMINOSITY-METALLICITY RELATION, COMPACT DWARF GALAXIES, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, DIGITAL SKY SURVEY, galaxies: abundances, Astrophysics::Earth and Planetary Astrophysics, GREEN PEA GALAXIES, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

Context. The study of large and representative samples of low-metallicity star-forming galaxies at different cosmic epochs is of great interest to the detailed understanding of the assembly history and evolution of low-mass galaxies. Aims. We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 Methods. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging, and optical zCOSMOS spectroscopy to derive the main global properties of star-forming EELGs, such as sizes, stellar masses, star formation rates (SFR), and reliable oxygen abundances using both "direct" and "strong-line" methods. Results. The EELGs are extremely compact (r(50) similar to 1.3 kpc), low-mass (M-* similar to 10(7)-10(10) M-circle dot) galaxies forming stars at unusually high specific star formation rates (sSFR equivalent to SFR/M-star up to 10(-7) yr(-1)) compared to main sequence star-forming galaxies of the same stellar mass and redshift. At rest-frame UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Ly alpha emitters, as revealed by GALEX spectroscopy. We show that zCOSMOS EELGs are high-ionization, low-metallicity systems, with median 12+log(O/H) = 8.16 +/- 0.21 (0.2 Z(circle dot)) including a handful of extremely metal-deficient ( Conclusions. The zCOSMOS EELGs are galaxies caught in a transient and probably early period of their evolution, where they are efficiently building up a significant fraction of their present-day stellar mass in an ongoing, galaxy-wide starburst. Therefore, the EELGs constitute an ideal benchmark for comparison studies between low- and high-redshift low-mass star-forming galaxies.

Published
2015

42. Hyperluminous starburst gives up its secrets.

Author

Ivison, R J, Page, M J, Cirasuolo, M, Harrison, C M, Mainieri, V, Arumugam, V, and Dudzevičiūtė, U

Subjects
SPECTRAL energy distribution, GRAVITATIONAL waves, ACTIVE galactic nuclei, SPECTRAL imaging, GALAXY clusters, SUPERMASSIVE black holes, QUANTUM information science, STARBURSTS
Abstract

HATLAS J084933.4 + 021443 was identified as a dusty starburst via its rest-frame far-infrared (far-IR) emission. Multifrequency imaging and spectroscopy revealed a cluster of four dusty galaxies at z  = 2.41, covering 80 kpc. Here, we use Atacama Large Millimetre Array to confirm a more distant, fifth protocluster member, and present X-ray and rest-frame optical imaging spectroscopy of the brightest, an unlensed hyperluminous IR galaxy (HyLIRG). The data reveal broad Hα and bright [N  ii ] lines, and bright X-ray emission, characteristics that betray a Type-1 active galactic nucleus (AGN), strengthening evidence that AGN are ubiquitous amongst HyLIRGs. The accreting black hole is supermassive, M bh ≈ 2 × 109 M⊙, with little intrinsic absorption, N H ≈ 5 × 1021 cm−2. The X-ray properties suggest the accretion luminosity rivals that of the starburst, yet it is not obvious where this emerges in its panchromatic spectral energy distribution. We outline three scenarios that could give rise to the observed characteristics, and how we might distinguish between them. In the first, we see the AGN through the host galaxy because of the cavity it excavates. In the others, the AGN is not cospatial with the starburst, having been ejected via asymmetric gravitational radiation, or having evolved towards the naked quasar phase in an unseen companion. [ABSTRACT FROM AUTHOR]

Published
2019
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43. Obscured AGN at 1.5 < z < 3.0 from the zCOSMOS-deep Survey: I. Properties of the emitting gas in the narrow-line region.

Author

Mignoli, M., Feltre, A., Bongiorno, A., Calura, F., Gilli, R., Vignali, C., Zamorani, G., Lilly, S. J., Le Fèvre, O., Bardelli, S., Bolzonella, M., Bordoloi, R., Le Brun, V., Caputi, K. I., Cimatti, A., Diener, C., Garilli, B., Koekemoer, A. M., Maier, C., and Mainieri, V.

Subjects
SEYFERT galaxies, STELLAR mass, ACTIVE galactic nuclei, IONIZED gases, GAS distribution, GALAXY spectra
Abstract

Context. The physics and demographics of high-redshift obscured active galactic nuclei (AGN) is still scarcely investigated. New samples of such objects, selected with different techniques, can provide useful insights into their physical properties. Aims. With the goal to determine the properties of the gas in the emitting region of type 2 AGN, in particular, the gas metal content, we exploit predictions from photoionization models, including new parameterizations for the distance of gas distribution from the central source and internal microturbulence in the emitting clouds, to interpret rest-frame UV spectral data. Methods. We selected a sample of 90 obscured (type 2) AGN with 1.45 ≤ z ≤ 3.05 from the zCOSMOS-deep galaxy sample by 5σ detection of the high-ionization C IVλ1549 narrow emission line. This feature in a galaxy spectrum is often associated with nuclear activity, and the selection effectiveness has also been confirmed by diagnostic diagrams based on utraviolet (UV) emission-line ratios. We applied the same selection technique and collected a sample of 102 unobscured (type 1) AGN. Taking advantage of the large amount of multiband data available in the COSMOS field, we investigated the properties of the C IV-selected type 2 AGN, focusing on their host galaxies, X-ray emission, and UV emission lines. Finally, we investigated the physical properties of the ionized gas in the narrow-line region (NLR) of this type 2 AGN sample by combining the analysis of strong UV emission lines with predictions from photoionization models. Results. We find that in order to successfully reproduce the relative intensity of UV emission lines of the selected high-z type 2 AGN, two new ingredients in the photoionization models are fundamental: small inner radii of the NLR (≈90 pc for LAGN = 1045 erg s−1), and the internal dissipative microturbulence of the gas-emitting clouds (with vmicr ≈ 100 km s−1). With these modified models, we compute the gas-phase metallicity of the NLR, and our measurements indicate a statistically significant evolution of the metal content with redshift. Finally, we do not observe a strong relationship between the NLR gas metallicity and the stellar mass of the host galaxy in our C IV-selected type 2 AGN sample. [ABSTRACT FROM AUTHOR]

Published
2019
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44. Prevalence of radio jets associated with galactic outflows and feedback from quasars.

Author

Jarvis, M E, Harrison, C M, Thomson, A P, Circosta, C, Mainieri, V, Alexander, D M, Edge, A C, Lansbury, G B, Molyneux, S J, and Mullaney, J R

Subjects
QUASARS, RADIO galaxies, IONIZED gases, RADIOS, STAR formation, ACTIVE galaxies
Abstract

We present 1–7 GHz high-resolution radio imaging (VLA and e-MERLIN) and spatially resolved ionized gas kinematics for 10 z < 0.2 type 2 'obscured' quasars (log [ L AGN/erg s−1] ≳ 45) with moderate radio luminosities (⁠|$\log [L_{\rm {1.4\,GHz}}$| /W Hz−1]  = 23.3–24.4). These targets were selected to have known ionized outflows based on broad [O  iii ] emission-line components (full width at half-maximum ≈ 800–1800 km s−1). Although 'radio-quiet' and not 'radio AGN' by many traditional criteria, we show that for nine of the targets, star formation likely accounts for ≲10 per cent of the radio emission. We find that ∼80–90 per cent of these nine targets exhibit extended radio structures on 1–25 kpc scales. The quasars' radio morphologies, spectral indices, and position on the radio size–luminosity relationship reveals that these sources are consistent with being low power compact radio galaxies. Therefore, we favour radio jets as dominating the radio emission in the majority of these quasars. The radio jets we observe are associated with morphologically and kinematically distinct features in the ionized gas, such as increased turbulence and outflowing bubbles, revealing jet–gas interaction on galactic scales. Importantly, such conclusions could not have been drawn from current low-resolution radio surveys such as FIRST. Our observations support a scenario where compact radio jets, with modest radio luminosities, are a crucial feedback mechanism for massive galaxies during a quasar phase. [ABSTRACT FROM AUTHOR]

Published
2019
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45. Multi-phase outflows in Mkn 848 observed with SDSS-MaNGA integral field spectroscopy.

Author

Perna, M., Cresci, G., Brusa, M., Lanzuisi, G., Concas, A., Mainieri, V., Mannucci, F., and Marconi, A.

Subjects
INTEGRAL field spectroscopy, GALAXY formation, BIPOLAR outflows (Astrophysics), GALACTIC evolution
Abstract

Aims. The characterisation of galaxy-scale outflows in terms of their multi-phase and multi-scale nature, amount, and effects of flowing material is crucial to place constraints on models of galaxy formation and evolution. This study can proceed only with the detailed investigation of individual targets. Methods. We present a spatially resolved spectroscopic optical data analysis of Mkn 848, a complex system consisting of two merging galaxies at z ∼ 0.04 that are separated by a projected distance of 7.5 kpc. Motivated by the presence of a multi-phase outflow in the north-west system revealed by the SDSS integrated spectrum, we analysed the publicly available MaNGA data, which cover almost the entire merging system, to study the kinematic and physical properties of cool and warm gas in detail. Results. Galaxy-wide outflowing gas in multiple phases is revealed for the first time in the two merging galaxies. We also detect spatially resolved resonant Na ID emission associated with the outflows. The derived outflow energetics (mass rate, and kinetic and momentum power) may be consistent with a scenario in which both winds are accelerated by stellar processes and AGN activity, although we favour an AGN origin given the high outflow velocities and the ionisation conditions observed in the outflow regions. Further deeper multi-wavelength observations are required, however, to better constrain the nature of these multi-phase outflows. Outflow energetics in the North-West system are strongly different between the ionised and atomic gas components, the latter of which is associated with mass outflow rate and kinetic and momentum powers that are one or two dex higher; those associated with the south-east galaxy are instead similar. Conclusions. Strong kiloparsec-scale outflows are revealed in an ongoing merger system, suggesting that feedback can potentially impact the host galaxy even in the early merger phases. The characterisation of the neutral and ionised gas phases has proved to be crucial for a comprehensive study of the outflow phenomena. [ABSTRACT FROM AUTHOR]

Published
2019
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46. Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in the XMM -COSMOS survey

Author

Lusso, E., Comastri, A., Simmons, B. D., Mignoli, M., Zamorani, G., Vignali, C., Brusa, M., Shankar, F., Lutz, D., Trump, J. R., Maiolino, R., Gilli, R., Bolzonella, M., Puccetti, S., Salvato, M., Impey, C. D., Civano, F., Elvis, M., Mainieri, V., Silverman, J. D., Koekemoer, A. M., Bongiorno, A., Merloni, A., Berta, S., Floc'h, E. Le, Magnelli, B., Pozzi, F., Riguccini, L., INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), AUTRES, INAF - Osservatorio Astronomico di Capodimonte (OAC), Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), INAF - Osservatorio Astronomico di Bologna (OABO), Università di Bologna, Dipartimento di Astronomia, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Space Telescope Science Institute (STSci), Max-Planck-Institut für Astrophysik (MPA), Ecosystèmes lagunaires : organisation biologique et fonctionnement (ECOLAG), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Lusso E., Comastri A., Simmons B.D., Mignoli M., Zamorani G., Vignali C., Brusa M., Shankar F., Lutz D., Trump J.R., Maiolino R., Gilli R., Bolzonella M., Puccetti S., Salvato M., Impey C.D., Civano F., Elvis M., Mainieri V., Silverman J.D., Koekemoer A.M., Bongiorno A., A. Merloni, Berta S., Le Floc'h E., Magnelli B., Pozzi F., Riguccini L., Harvard University-Smithsonian Institution, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Galaxies: active, Galaxies: evolution, Methods: statistical, Quasars: general, Astronomy and Astrophysics, Space and Planetary Science, [PHYS]Physics [physics], methods: statistical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, quasars: general, Astrophysics::Solar and Stellar Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Bolometric luminosities and Eddington ratios of both X-ray selected broad-line (Type-1) and narrow-line (Type-2) AGN from the XMM-Newton survey in the COSMOS field are presented. The sample is composed by 929 AGN (382 Type-1 AGN and 547 Type-2 AGN) and it covers a wide range of redshifts, X-ray luminosities and absorbing column densities. About 65% of the sources are spectroscopically identified as either Type-1 or Type-2 AGN (83% and 52% respectively), while accurate photometric redshifts are available for the rest of the sample. The study of such a large sample of X-ray selected AGN with a high quality multi-wavelength coverage from the far-infrared (now with the inclusion of Herschel data at 100 micron and 160 micron) to the optical-UV allows us to obtain accurate estimates of bolometric luminosities, bolometric corrections and Eddington ratios. The kbol-Lbol relations derived in the present work are calibrated for the first time against a sizable AGN sample, and rely on observed redshifts, X-ray luminosities and column density distributions. We find that kbol is significantly lower at high Lbol with respect to previous estimates by Marconi et al. (2004) and Hopkins et al. (2007). Black hole masses and Eddington ratios are available for 170 Type-1 AGN, while black hole masses for Type-2 AGN are computed for 481 objects using the black hole mass-stellar mass relation and the morphological information. We confirm a trend between kbol and lambda_Edd, with lower hard X-ray bolometric corrections at lower Eddington ratios for both Type-1 and Type-2 AGN. We find that, on average, Eddington ratio increases with redshift for all Types of AGN at any given Mbh, while no clear evolution with redshift is seen at any given Lbol., Comment: 19 pages, 18 figures, accepted to MNRAS

Published
2012
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47. The COSMOS Density Field: A Reconstruction Using Both Weak Lensing and Galaxy Distributions

Author

Amara, A., Lilly, S., Kovac, K., Rhodes, J., Massey, R., Zamorani, G., Carollo, C. M., Contini, T., Kneib, J-P, Le Fevre, O., Mainieri, V., Renzini, A., Scodeggio, M., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Cucciati, O., Torre, S., Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Lamareille, F., Le Borgne, J-F, Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Presotto, V., Silverman, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., BARNES, L., Bordoloi, R., Cappi, A., Cimatti, Alessandro, Coppa, G., Koekoemoer, A., Lopez-Sanjuan, C., McCracken, H. J., Moresco, M., Nair, P., Pozzetti, L., Welikala, N., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Amara A., Lilly S., Kovač K., Rhodes J., Massey R., Zamorani G., Carollo C. M., Contini T., Kneib J.-P., Le Fevre O., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Peng Y., Montero E. Perez, Presotto V., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Barnes L., Bordoloi R., Cappi A., Cimatti A., Coppa G., Koekoemoer A., López-Sanjuan C., McCracken H. J., Moresco M., Nair P., Pozzetti L., Welikala N., Astronomy, and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
SAMPLE, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], DEEP, DATA RELEASE, FOS: Physical sciences, HUBBLE-SPACE-TELESCOPE, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter, ADVANCED CAMERA, Large-scale structure of Universe, LARGE-SCALE STRUCTURE, DARK-MATTER, Dark matter, DIGITAL SKY SURVEY, dark matter, large-scale structure of Universe, large-scale structure of Universe, CLUSTERS, ZCOSMOS GALAXIES, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The COSMOS field has been the subject of a wide range of observations, with a number of studies focusing on reconstructing the 3D dark matter density field. Typically, these studies have focused on one given method or tracer. In this paper, we reconstruct the distribution of mass in the COSMOS field out to a redshift z=1 by combining Hubble Space Telescope weak lensing measurements with zCOSMOS spectroscopic measurements of galaxy clustering. The distribution of galaxies traces the distribution of mass with high resolution (particularly in redshift, which is not possible with lensing), and the lensing data empirically calibrates the mass normalisation (bypassing the need for theoretical models). Two steps are needed to convert a galaxy survey into a density field. The first step is to create a smooth field from the galaxy positions, which is a point field. We investigate four possible methods for this: (i) Gaussian smoothing, (ii) convolution with truncated isothermal sphere, (iii) fifth nearest neighbour smoothing and (iv) a muliti-scale entropy method. The second step is to rescale this density field using a bias prescription. We calculate the optimal bias scaling for each method by comparing predictions from the smoothed density field with the measured weak lensing data, on a galaxy-by-galaxy basis. In general, we find scale-independent bias for all the smoothing schemes, to a precision of 10%. For the nearest neighbour smoothing case, we find the bias to be 2.51\pm 0.25. We also find evidence for a strongly evolving bias, increasing by a factor of ~3.5 between redshifts 0, Comment: Accepted by MNRAS. 12 pages with 6 Figures

Published
2012
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48. Spectral energy distributions of Type~1 AGN in the COSMOS survey I - The XMM-COSMOS sample

Author

Elvis M., Hao H., Civano F., Salvato M., Bongiorno A., Capak P., Zamorani G., Comastri A., Jahnke K., Mainieri V., Trump J. R., Ho L. C., Aussel A., Cappelluti N., Cisternas M., Frayer D., Gilli R., Hasinger G., Huchra J. P., Impey C. D., Koekemoer A. M., LANZUISI, GIORGIO, Le Floc'h E., Lilly S. J., Liu Y., McCarthy P., McCracken H. J., Merloni A., Roeser H. J., Sanders D. B., Sargent M., Scoville N., Schinnerer E., Schiminovich D., Silverman J., Taniguchi Y., Urry C. M., Zamojski M. A., Zatloukal M., BRUSA, MARCELLA, LUSSO, ELISABETA, VIGNALI, CRISTIAN, Elvis M., Hao H., Civano F., Brusa M., Salvato M., Bongiorno A., Capak P., Zamorani G., Comastri A., Jahnke K., Lusso E., Mainieri V., Trump J.R., Ho L.C., Aussel A., Cappelluti N., Cisternas M., Frayer D., Gilli R., Hasinger G., Huchra J.P., Impey C.D., Koekemoer A.M., Lanzuisi G., Le Floc'h E., Lilly S.J., Liu Y., McCarthy P., McCracken H.J., Merloni A., Roeser H.-J., Sanders D.B., Sargent M., Scoville N., Schinnerer E., Schiminovich D., Silverman J., Taniguchi Y., Vignali C., Urry C.M., Zamojski M.A., and Zatloukal M.

Subjects
surveys, Astrophysics::High Energy Astrophysical Phenomena, quasars: general, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

The "Cosmic Evolution Survey" (COSMOS) enables the study of the spectral energy distributions (SEDs) of active galactic nuclei (AGNs) because of the deep coverage and rich sampling of frequencies from X-ray to radio. Here we present an SED catalog of 413 X-ray (XMM-Newton)-selected type 1 (emission line FWHM > 2000 km s-1) AGNs with Magellan, SDSS, or VLT spectrum. The SEDs are corrected for Galactic extinction, broad emission line contributions, constrained variability, and host galaxy contribution. We present the mean SED and the dispersion SEDs after the above corrections in the rest-frame 1.4 GHz to 40 keV, and show examples of the variety of SEDs encountered. In the near-infrared to optical (rest frame ~8 μm-4000 Å), the photometry is complete for the whole sample and the mean SED is derived from detections only. Reddening and host galaxy contamination could account for a large fraction of the observed SED variety. The SEDs are all available online.

Published
2012

49. Accreting supermassive black holes in the COSMOS Field and the connection to their host galaxies

Author

Bongiorno A., Merloni A., Magnelli B., Salvato M., Mignoli M., Zamorani G., Fiore F., Rosario D., Mainieri V., Comastri A., Balestra I., Bardelli S., Berta S., Civano F., Kampczyk P., Le Floc'h E., Lutz D., Pozzetti L., Riguccini L., Shankar F., Silverman J., BRUSA, MARCELLA, VIGNALI, CRISTIAN, LUSSO, ELISABETA, POZZI, FRANCESCA, Bongiorno A., Merloni A., Brusa M., Magnelli B., Salvato M., Mignoli M., Zamorani G., Fiore F., Rosario D., Mainieri V., Comastri A., Vignali C., Balestra I., Bardelli S., Berta S., Civano F., Kampczyk P., Le Floc'h E., Lusso E., Lutz D., Pozzetti L., Pozzi F., Riguccini L., Shankar F., and Silverman J.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, survey, galaxies: fundamental parameters, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

Using the wide multiband photometry available in the Cosmic Evolution Survey (COSMOS) field, we explore the host galaxy properties of a large sample of active galactic nuclei (AGNs; ˜1700 objects) with Lbol ranging from 1043 to 1047 erg s-1, obtained by combining X-ray and optical spectroscopic selections. Based on a careful study of their spectral energy distributions, which have been parametrized using a two-component (AGN+galaxy) model fit, we have derived dust-corrected rest-frame magnitudes, colours and stellar masses of the obscured and unobscured AGN hosts up to high redshift (z≲3). Moreover, for the sample of obscured AGNs, we have also derived reliable star formation rates (SFRs). We find that AGN hosts span a large range of stellar masses and SFRs. No colour-bimodality is seen at any redshift in the AGN hosts, which are found to be mainly massive, red galaxies. Once we have accounted for the colour-mass degeneracy in well-defined mass-matched samples, we find a residual (marginal) enhancement of the incidence of AGNs in redder galaxies with lower specific SFRs. We argue that this result might emerge because of our ability to properly account for AGN light contamination and dust extinction, compared to surveys with a more limited multiwavelength coverage. However, because these colour shifts are relatively small, systematic effects could still be considered responsible for some of the observed trends. Interestingly, we find that the probability for a galaxy to host a black hole that is growing at any given 'specific accretion rate' (i.e. the ratio of X-ray luminosity to the host stellar mass) is almost independent of the host galaxy mass, while it decreases as a power law with LX/M*. By analysing the normalization of such a probability distribution, we show how the incidence of AGNs increases with redshift as rapidly as (1 + z)4, which closely resembles the overall evolution of the specific SFR of the entire galaxy population. We provide analytical fitting formulae that describe the probability of a galaxy of any mass (above the completeness limit of the COSMOS) to host an AGN of any given specific accretion rate as a function of redshift. These can be useful tools for theoretical studies of the growing population of black holes within galaxy evolution models. Although AGN activity and star formation in galaxies do appear to have a common triggering mechanism, at least in a statistical sense, within the COSMOS sample, we do not find any conclusive evidence to suggest that AGNs have a powerful influence on the star-forming properties of their host galaxies.

Published
2012

50. The radio-X-ray relation as a star formation indicator: results from the Very Large Array-Extended Chandra Deep Field-South

Author

Vattakunnel, Shaji, Tozzi, P., Matteucci, MARIA FRANCESCA, Padovani, P., Miller, N., Bonzini, M., Mainieri, V., Paolillo, M., Vincoletto, L., Brandt, W. N., Luo, B., Kellermann, K. I., Xue, Y. Q., Vattakunnel, Shaji, Tozzi, P., Matteucci, MARIA FRANCESCA, Padovani, P., Miller, N., Bonzini, M., Mainieri, V., Paolillo, M., Vincoletto, L., Brandt, W. N., Luo, B., Kellermann, K. I., Xue, Y. Q., S., Vattakunnel, P., Tozzi, F., Matteucci, P., Padovani, N., Miller, M., Bonzini, V., Mainieri, Paolillo, Maurizio, L., Vincoletto, W. N., Brandt, B., Luo, K. I., Kellermann, and Y. Q., Xue

Subjects
X-rays: galaxies, cosmology: observation, galaxies: active, galaxies: star formation, cosmology: observations, active [galaxies], star formation [galaxies], observation [cosmology], galaxies [X-rays]
Abstract

In order to trace the instantaneous star formation rate (SFR) at high redshift, and thus help in understanding the relation between the different emission mechanisms related to star formation, we combine the recent 4-Ms Chandra X-ray data and the deep Very Large Array radio data in the Extended Chandra Deep Field-South region. We find 268 sources detected both in the X-ray and radio bands. The availability of redshifts for {\tilde}95 per cent of the sources in our sample allows us to derive reliable luminosity estimates and the intrinsic properties from X-ray analysis for the majority of the objects. With the aim of selecting sources powered by star formation in both bands, we adopt classification criteria based on X-ray and radio data, exploiting the X-ray spectral features and time variability, taking advantage of observations scattered across more than 10 years. We identify 43 objects consistent with being powered by star formation. We also add another 111 and 70 star-forming candidates detected only in the radio and X-ray bands, respectively. We find a clear linear correlation between radio and X-ray luminosity in star-forming galaxies over three orders of magnitude and up to z{\tilde} 1.5. We also measure a significant scatter of the order of 0.4 dex, higher than that observed at low redshift, implying an intrinsic scatter component. The correlation is consistent with that measured locally, and no evolution with redshift is observed. Using a locally calibrated relation between the SFR and the radio luminosity, we investigate the L$_{X}$(2-10 keV)-SFR relation at high redshift. The comparison of the SFR measured in our sample with some theoretical models for the Milky Way and M31, two typical spiral galaxies, indicates that, with current data, we can trace typical spirals only at z{\le} 0.2, and strong starburst galaxies with SFRs as high as {\tilde}100 M$_{&sun;}$ yr$^{-1}$, up to z{\tilde} 1.5.

Published
2012

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