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Papers

Circosta et al. (2018). "SUPER I. Toward an unbiased study of ionised outflows in z~2 active galactic nuclei: survey overview and sample characterisation"

This paper introduce the survey and describe the targets selection criteria. It presents also a full characterisation of the multi-wavelength properties of each target. Spectral energy distribution fitting of UV-to-FIR photometry was used to derive stellar masses (4 × 109 - 2 × 1011 M☉), star formation rates (25 - 680 M☉ yr-1) and AGN bolometric luminosities (2 × 1044 - 8 × 1047 erg s-1). In addition, X-ray spectral analysis was used to measure the obscuring column densities (up to 2 × 1024 cm-2) and luminosities in the hard 2 - 10 keV band (2 × 1043 - 6 × 1045 erg s-1). Finally, we classify our AGN as jetted or non-jetted according to their radio and FIR emission.

Two examples of rest-frame SEDs obtained for a type 2 (XID522, left) and a type 1 (cid_166, right) AGN. The black dots represent the observed multi-wavelength photometry, while the empty dots indicate 3σ upper limits. The black solid line is the total best-fit model, the orange curve represents the stellar emission attenuated by dust, the green template reproduces the AGN emission, the red curve accounts for dust emission heated by star formation. Emission lines in the black curves are part of the nebular emission component, included in the overall SED. Figure from Circosta et al. (2018).
Distribution of host galaxy properties in the SFR-M* plane for the 24 AGN (type 1s marked by triangles and type 2s marked by circles) with star formation constraints in our sample. The two data points with green edges represent the targets with SFR derived through modeling of the stellar emission with SED fitting. The color coding indicates the AGN bolometric luminosity for each object of this subsample. The black solid line reproduces the main sequence (MS) of star-forming galaxies from Schreiber et al. (2015) at the average redshift of our target sample (i.e. ∼2.3). The dashed lines mark the scatter of the main sequence (equal to 0.3 dex) while the dot-dashed line represents the locus 4 times above the main sequence along the SFR axis (as defined by Rodighiero et al. 2011). The gray squares trace the properties of the 25 star-forming galaxies targeted by the SINS/zC-SINF survey (Förster Schreiber et al. 2018) without AGN signatures. Figure from Circosta et al. (2018).

 

Kakkad et al. (2020) "SUPER II. Spatially resolved ionised gas kinematics and scaling relations in z~2 AGN host galaxies"

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. 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%.

Inverse cumulative w80 distribution measured for [O III] λ5007 line, for AGN and star forming samples from different surveys. The AGN sample consists of targets from the SUPER survey in red (this paper) and targets from KASHz survey matched in redshift in black (Harrison et al. 2016). The Type 1 sample used in this paper has a median hard X-ray luminosity of 1044.8 erg s−1 and the redshift-matched KASHz targets have a median X-ray luminosity of 1043.9 erg s−1. The blue line shows the w80 distribution of mass-matched low redshift star forming sample from Wylezalek et al. (2020). The dashed black-line at 600 km s−1 corresponds to the w80 value used in this work to define if a target hosts an AGN-driven outflow. Figure adapted from Kakkad et al. (2020).
Ionised gas [O III] mass outflow rate versus bolometric luminosity of AGN for the SUPER Type 1 sample presented in this paper and literature data of low- and high-redshift AGN. The red shaded area and the black hatched area show the mass outflow rates for the SUPER targets assuming a biconical outflow model and a thin-shell model. The green shaded area shows the outflow rates for ionised gas from literature data compiled in Fiore et al. (2017) (after rescaling the relation with the same assumption as the Type 1 SUPER targets, see Sect. 5.5) and the blue shaded region shows the outflow rates for low redshift X-ray AGN sample from Davies et al. (2020b). The shaded region in all the studies correspond to mass outflow rates assuming an electron density from 500 cm−3–10 000 cm−3. Figure from Kakkad et al. (2020).

 

 

 

 

Vietri et al. (2020). Broad Line Region properties of AGN at z~2

The main aims of this paper were: (a) to derive reliable estimates for the masses of the black holes and accretion rates for the Type-1 AGNs in this survey; and (b) to characterise the properties of the AGN-driven winds in the broad line region (BLR). Concerning the last point, we confirm that the CIV line width does not correlate with the Balmer lines and its peak is blueshifted with respect to the [OIII]-based systemic redshift. We interpreted this findings as the presence of outflows in the BLR with derived velocities up to ∼4700 km s−1. We derive mass outflows rates in the range 0.005–3 M⊙ yr−1 for the BLR winds. The mass outflow rate of the BLR winds shows a correlation with bolometric luminosity as steep as that observed for winds at sub-parsec scale distances and in the NLR. The kinetic power of the BLR winds inferred is Ėkin∼ 10[ − 7 : −4] × Lbol, and in 28% of the SUPER sample the kinetic power of the BLR and NLR winds are comparable.

Bolometric luminosity as a function of BH mass, both in logarithmic scale, for the SUPER sample. Luminosity in fractions of 0.1, 0.5, and 1 Eddington luminosity are respectively indicated with dot-dashed, dotted, and dashed lines. Contours and grey points refer to SDSS DR7 QSOs from Shen et al. (2011). Figure from Vietri et al. (2020)

 

We derive mass outflows rates in the range 0.005–3 M⊙ yr−1 for the BLR winds. The mass outflow rate of the BLR winds shows a correlation with bolometric luminosity as steep as that observed for winds at sub-parsec scale distances and in the NLR. The kinetic power of the BLR winds inferred is Ėkin ∼ 10[ − 7 : −4] × Lbol, and in 28% of the SUPER sample the kinetic power of the BLR and NLR winds are comparable. Figure from Vietri et al. (2020)
Circosta et al. (2021). CO(J=3-2) properties of active galactic nucleus hosts at cosmic noon revealed by ALMA

In this paper we present the first systematic study of the CO properties of AGN hosts at z~2 for a sample of 27 X-ray selected AGN spanning two orders of magnitude in AGN bolometric luminosity (Lbol= 10^44.7-10^46.9 erg/s) by using ALMA Band 3 observations of the CO(3-2) transition (~1" angular resolution). To search for evidence of AGN feedback on the CO properties of the host galaxies, we compared our AGN with a sample of inactive (i.e., non-AGN) galaxies from the PHIBSS survey with similar redshift, stellar masses, and SFRs. The two samples show statistically consistent trends in the LCO(3-2)-Lfir and LCO(3-2)-M* planes. However, there are indications that AGN feature lower CO(3-2) luminosities (0.4-0.7 dex) than inactive galaxies at the 2-3sigma level when we focus on the subset of parameters where the results are better constrained and on the distribution of the mean LCO(3-2)/M*. Therefore, even by conservatively assuming the same excitation factor r31, we would find lower molecular gas masses in AGN, and assuming higher r31 would exacerbate this difference. We interpret our result as a hint of the potential effect of AGN activity (e.g., radiation and outflows), which may be able to heat, excite, dissociate, and/or deplete the gas reservoir of the host galaxies.

Distribution of the ratio between L′ CO and stellar mass (proxy of gas fraction) for AGN (red) and inactive galaxies (blue). The filled histograms show the sampled posterior distribution of the mean (μ) of the hierarchical Gaussian prior adopted in our Bayesian analysis. In the bottom part of the plot, individual detections and upper lim- its are displayed. The unfilled histograms represent the total distribu- tions and were obtained by joining the sampled posterior distributions of each target in the AGN or inactive galaxy sample. AGN show a mean log(L′ /M∗) of −1.39+0.23, while for inactive galaxies we find CO −0.30 −0.82+0.14 . The log(L′ /M∗ ) ratio of AGN is lower than inactive galax- −0.11 CO ies by a factor ∼3.7 (0.57 dex), at the 2.2σ level. The two distributions are significantly different, as confirmed by statistical tests. Figure from Circosta et al. (2021).

 

 

 

Lamperti et al. 2021. ALMA continuum observations of z~2 AGN and the elusive evidence of outflows influencing star formation.

We used high resolution ALMA Band-7 continuum observations of wight AGN from SUPER to study the impact that AGN outflows may have on the dust properties, and possibly star-formation of the hosts. The majority of our sample show different morphologies for the FIR (mostly due to reprocessed stellar emission) and the ionised gas emission (Hα and [O iii], mostly due to AGN emission). Under the assumption that the FIR emission is a reliable tracer of obscured star formation, we find that the obscured star formation activity in these AGN host galaxies is not clearly affected by the ionised outflows. However, we cannot rule out that star formation suppression is happening on smaller spatial scales than the ones we probe with our observations (< 2 kpc) or on different timescales.

Maps of [Oiii] emission in three different velocity channels: blue-shifted emission (< -300 km s−1, first column), central channel ([-300, 300] km s−1, second column), red-shifted emission (> 300 km s−1, third column). The interval over which the spectrum has been integrated is indicated on the right plot. In black are the [O iii] emission contours starting from 2σ and increas- ing in intervals of 1σ. In white are the FIR emission contours, starting from 2σ and increasing in intervals of 2σ (or intervals of 4σ for X_N_81_44 and cid_346, to improve presentation). Negative -2σ contours are shown with dashed curves. The grey ellipse shows the size of the ALMA beam, while the white scale-bar shows the size of the PSF of the [O iii] image in kpc. The blue cross and circle show the position and uncertainty of the optical continuum. Fourth column: spectrum around the [O iii]λ5007 emission line. The coloured areas show the spectral regions over which the emission was integrated to create the three images on the left.

Cicone et al. 2021. A giant molecular halo around a z~2 quasar.

In this work we present the discovery of a gigantic molecular gas halo around cid346, a z=2.2 quasar studied as part of SUPER. New Atacama Compact Array (ACA) CO(3-2) observations detect a much higher flux (by a factor of 14±5) than measured on kpc-scales (r≲8 kpc) using previous snapshot Atacama Large Millimeter/submillimeter Array (ALMA) data. Such additional CO(3-2) emission traces a structure that extends out to r∼200 kpc in projected size. This is the most extended molecular circumgalactic medium (CGM) reservoir that has ever been mapped. Since cid346 hosts AGN-driven ionized outflows and since there is no evidence of merging companions or an overdensity, we suggest that outflows may have played a crucial rule in seeding metal-enriched, dense gas on halo scales. However, the origin of such an extended molecular CGM remains unclear.

ACA map obtained by integrating the CO(3-2) line emis- sion within −400 < v[km s−1] < 1000. For visualization pur- poses, the map has not been divided by the primary beam pro- file, hence the noise is uniform across the field. Negative con- tours are shown as dashed curves. Both negative and positive contours are plotted in steps of 1σ starting from ±1σ, with 1σ = 0.33 mJy beam−1. The phase center is indicated with a black cross and corresponds to the AGN position.