An outflow in the Seyfert ESO 362-G18 revealed by Gemini-GMOS/IFU observations

Indexación: Scopus.We present two-dimensional stellar and gaseous kinematics of the inner 0.7 × 1.2 kpc2 of the Seyfert 1.5 galaxy ESO 362-G18, derived from optical (4092-7338 Å) spectra obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of ≈ 170 pc and spectral resolution of 36 km s-1. ESO 362-G18 is a strongly perturbed galaxy of morphological type Sa or S0/a, with a minor merger approaching along the NE direction. Previous studies have shown that the [O III] emission shows a fan-shaped extension of ≈ 10′′ to the SE. We detect the [O III] doublet, [N II] and Hα emission lines throughout our field of view. The stellar kinematics is dominated by circular motions in the galaxy plane, with a kinematic position angle of ≈ 137° and is centred approximately on the continuum peak. The gas kinematics is also dominated by rotation, with kinematic position angles ranging from 122° to 139°, projected velocity amplitudes of the order of 100 km s-1, and a mean velocity dispersion of 100 km s-1. A double-Gaussian fit to the [O III]λ5007 and Hα lines, which have the highest signal to noise ratios of the emission lines, reveal two kinematic components: (1) a component at lower radial velocities which we interpret as gas rotating in the galactic disk; and (2) a component with line of sight velocities 100-250 km s-1 higher than the systemic velocity, interpreted as originating in the outflowing gas within the AGN ionization cone. We estimate a mass outflow rate of 7.4 × 10-2 M⊙ yr-1 in the SE ionization cone (this rate doubles if we assume a biconical configuration), and a mass accretion rate on the supermassive black hole (SMBH) of 2.2 × 10-2 M⊙ yr-1. The total ionized gas mass within ∼84 pc of the nucleus is 3.3 × 105 M⊙; infall velocities of ∼34 km s-1 in this gas would be required to feed both the outflow and SMBH accretion. © ESO 2018.https://www.aanda.org/articles/aa/abs/2018/06/aa31671-17/aa31671-17.htm

Observing Supermassive Black Holes across cosmic time: from phenomenology to physics

In the last decade, a combination of high sensitivity, high spatial resolution observations and of coordinated multi-wavelength surveys has revolutionized our view of extra-galactic black hole (BH) astrophysics. We now know that supermassive black holes reside in the nuclei of almost every galaxy, grow over cosmological times by accreting matter, interact and merge with each other, and in the process liberate enormous amounts of energy that influence dramatically the evolution of the surrounding gas and stars, providing a powerful self-regulatory mechanism for galaxy formation. The different energetic phenomena associated to growing black holes and Active Galactic Nuclei (AGN), their cosmological evolution and the observational techniques used to unveil them, are the subject of this chapter. In particular, I will focus my attention on the connection between the theory of high-energy astrophysical processes giving rise to the observed emission in AGN, the observable imprints they leave at different wavelengths, and the methods used to uncover them in a statistically robust way. I will show how such a combined effort of theorists and observers have led us to unveil most of the SMBH growth over a large fraction of the age of the Universe, but that nagging uncertainties remain, preventing us from fully understating the exact role of black holes in the complex process of galaxy and large-scale structure formation, assembly and evolution.Comment: 46 pages, 21 figures. This review article appears as a chapter in the book: "Astrophysical Black Holes", Haardt, F., Gorini, V., Moschella, U and Treves A. (Eds), 2015, Springer International Publishing AG, Cha

Quasars and their host galaxies

This review attempts to describe developments in the fields of quasar and quasar host galaxies in the past five. In this time period, the Sloan and 2dF quasar surveys have added several tens of thousands of quasars, with Sloan quasars being found to z>6. Obscured, or partially obscured quasars have begun to be found in significant numbers. Black hole mass estimates for quasars, and our confidence in them, have improved significantly, allowing a start on relating quasar properties such as radio jet power to fundamental parameters of the quasar such as black hole mass and accretion rate. Quasar host galaxy studies have allowed us to find and characterize the host galaxies of quasars to z>2. Despite these developments, many questions remain unresolved, in particular the origin of the close relationship between black hole mass and galaxy bulge mass/velocity dispersion seen in local galaxies.Comment: Review article, to appear in Astrophysics Update

Outflowing gas in a compact ionization cone in the Seyfert 2 galaxy ESO 153-G20

Contains fulltext : 208877.pdf (publisher's version ) (Open Access

Atlas of Quasar Energy Distributions - Digital Datasets

Tables and supplementary material from the Atlas of Quasar Energy Distributions, including tabulated estimates for median and quantile SEDs, given as log (nu Lnu) vs log(nu), for the sample of quasars. The SEDs are in the 'med' subdirectory. You probably want to start with 'med/MED.Median' which gives the median SED for the sample in log (nu Lnu) vs log(nu) normalized at 1.5 microns

ESO 362-G18 datacube

The observations were obtained with the integral field unit of the Gemini Multi-Object Spectrograph (GMOS-IFU) at the Gemini South telescope on the night of December 23, 2014 (Gemini projec

ESO 362-G18 datacube

Item does not contain fulltextThe observations were obtained with the integral field unit of the Gemini Multi-Object Spectrograph (GMOS-IFU) at the Gemini South telescope on the night of December 23, 2014 (Gemini projec

Lonely online: a social model of digital media addiction: a study in 21 countries

Digital media addiction limits face-to-face communication, which can have negative effects on the subjective wellbeing of individuals. However, the effect of digital media addiction on subjective wellbeing has not been adequately explored, and it is recommended in the literature that the role of mediating variables related to social life should be investigated. These include loneliness and satisfaction with relationships. The current study investigated whether loneliness and satisfaction with relationships explained the link between people’s digital media addiction and their sense of flourishing. A sample of 6,434 respondents from 21 countries (Mage = 25.92 years, SD = 9.78; 65.5% women) took part in a cross-sectional survey study. The study included a comprehensive evaluation of digital media addiction using several measures. The following scales were applied: the Internet Addiction Scale, the Facebook Intrusion Questionnaire, the Phubbing Scale, the De Jong Gierveld Loneliness Scale, the Relationship Assessment Scale, and the Flourishing Scale. A two-level path analysis showed that loneliness and satisfaction with interpersonal relationships fully mediated the link between digital media addiction and flourishing on the individual level. This suggests that digital media addiction may affect flourishing only through its impact on loneliness and satisfaction with interpersonal relationships.</p