We present Atacama Large Millimeter/submillimeter Array (ALMA) 860 μm imaging of four high-redshift (z = 2.8-5.7) dusty sources that were detected using the South Pole Telescope (SPT) at 1.4 mm and are not seen in existing radio to far-infrared catalogs. At 1."5 resolution, the ALMA data reveal multiple images of each submillimeter source, separated by 1"-3", consistent with strong lensing by intervening galaxies visible in near-IR imaging of these sources. We describe a gravitational lens modeling procedure that operates on the measured visibilities and incorporates self-calibration-like antenna phase corrections as part of the model optimization, which we use to interpret the source structure. Lens models indicate that SPT0346-52, located at z = 5.7, is one of the most luminous and intensely star-forming sources in the universe with a lensing corrected FIR luminosity of 3.7 × 10^(13) L_☉ and star formation surface density of 4200 M_☉ yr^(–1) kpc^(–2). We find magnification factors of 5 to 22, with lens Einstein radii of 1."1-2."0 and Einstein enclosed masses of 1.6-7.2 × 10^(11) M_☉. These observations confirm the lensing origin of these objects, allow us to measure their intrinsic sizes and luminosities, and demonstrate the important role that ALMA will play in the interpretation of lensed submillimeter sources.

/pdf/alma-observations-of-spt-discovered-strongly-lensed-dusty-1vuoqyw3ab.pdf

ALMA Observations of SPT-Discovered, Strongly Lensed, Dusty, Star-Forming Galaxies

At less than 4 Mpc distance the radio galaxy NGC 5128 (Centaurus A) is the prime example to study the supermassive black hole and its influence on the environment in great detail. To model and understand the feeding and feedback mechanisms one needs an accurate determination of the mass of the supermassive black hole. The aim of this review is to give an overview of the recent studies that have been dedicated to measure the black hole mass in Centaurus A from both gas and stellar kinematics. It shows how the advancement in observing techniques and instrumentation drive the field of black hole mass measurements and concludes that adaptive optics assisted integral field spectroscopy is the key to identify the effects of the AGN on the surrounding ionised gas. Using data from SINFONI at the ESO Very Large Telescope, the best-fit black hole mass is MBH = 4.5(+1.7,–1.0) × 107 M⊙ (from H2 kinematics) and MBH = (5.5 ± 3.0) × 107 M⊙ (from stellar kinematics). This is one of the cleanest gas-versus-star comparisons of a MBH determination, and brings Centaurus A into agreement with the MBH–σ relation.

/pdf/the-supermassive-black-hole-at-the-heart-of-centaurus-a-1utci5u5k5.pdf

The Supermassive Black Hole at the Heart of Centaurus A: Revealed by the Kinematics of Gas and Stars

At less than 4 Mpc distance the radio galaxy NGC 5128 (Centaurus A) is the prime example to study the supermassive black hole and its influence on the environment in great detail. To model and understand the feeding and feedback mechanisms one needs an accurate determination of the mass of the supermassive black hole. The aim of this review is to give an overview of the recent studies that have been dedicated to measure the black hole mass in Centaurus A from both gas and stellar kinematics. It shows how the advancement in observing techniques and instrumentation drive the field of black hole mass measurements and concludes that adaptive optics assisted integral field spectroscopy is the key to identify the effects of the AGN on the surrounding ionised gas. Using data from SINFONI at the ESO Very Large Telescope, the best-fit black hole mass is M_BH=4.5 +1.7/-1.0 x 10^7 Msolar (from H_2 kinematics) and M_BH= (5.5 +/- 3.0) x 10^7 Msolar (from stellar kinematics; both with 3 sigma errors). This is one of the cleanest gas vs star comparison of a M_BH determination, and brings Centaurus A into agreement with the M_BH-sigma relation.

/pdf/the-supermassive-black-hole-at-the-heart-of-centaurus-a-56b4hmq8aq.pdf

The Supermassive Black Hole at the Heart of Centaurus A: Revealed by Gas- and Stellar Kinematics

Supermassive black holes launching plasma jets at close to speed of light, producing gamma-rays, have ubiquitously been found to be hosted by massive elliptical galaxies. Since elliptical galaxies are generally believed to be built through galaxy mergers, active galactic nuclei (AGN) launching relativistic jets are associated to the latest stages of galaxy evolution. We have discovered a pseudo-bulge morphology in the host galaxy of the gamma-ray AGN PKS 2004-447. This is the first gamma-ray emitter radio loud AGN found to be launched from a system where both black hole and host galaxy have been actively growing via secular processes. This is evidence for an alternative black hole-galaxy co-evolutionary path to develop powerful relativistic jets that is not merger-driven.

/pdf/discovery-of-a-pseudobulge-galaxy-launching-powerful-3k703o2qth.pdf

Discovery of a pseudobulge galaxy launching powerful relativistic jets

We have obtained low-resolution optical (0.7-0.98 micron) and near-infrared (1.11-1.34 micron and 0.8-2.5 micron) spectra of twelve isolated planetary-mass candidates (J = 18.2-19.9 mag) of the 3-Myr sigma Orionis star cluster with a view to determining the spectroscopic properties of very young, substellar dwarfs and assembling a complete cluster mass function. We have classified our targets by visual comparison with high- and low-gravity standards and by measuring newly defined spectroscopic indices. We derived L0-L4.5 and M9-L2.5 using high- and low-gravity standards, respectively. Our targets reveal clear signposts of youth, thus corroborating their cluster membership and planetary masses (6-13 Mjup). These observations complete the sigma Orionis mass function by spectroscopically confirming the planetary-mass domain to a confidence level of $\sim$75 percent. The comparison of our spectra with BT-Settl solar metallicity model atmospheres yields a temperature scale of 2350-1800 K and a low surface gravity of log g ~ 4.0 [cm/s2], as would be expected for young planetary-mass objects. We discuss the properties of the cluster least-massive population as a function of spectral type. We have also obtained the first optical spectrum of S Ori 70, a T dwarf in the direction of sigma Orionis. Our data provide reference optical and near-infrared spectra of very young L dwarfs and a mass function that may be used as templates for future studies of low-mass substellar objects and exoplanets. The extrapolation of the sigma Orionis mass function to the solar neighborhood may indicate that isolated planetary-mass objects with temperatures of 200-300 K and masses in the interval 6-13-Mjup may be as numerous as very low-mass stars.

Optical and Near-Infrared Spectra of sigma Orionis Isolated Planetary-mass Objects

ISAAC sees first light at the VLT.

A number of articles have recently appeared in the ESO Messenger reporting on the past experience of the NTT service observing programme in Periods 58, 59 and 60 (Silva and Quinn 1997, Silva 1998). In this paper, the third in this series, we report on the results of a statistical analysis of the efficiency of service observing during Period 60. We have compared service observing (SO) with the classical ‘Visitor’ Mode (VIS), and with the other main programme executed at the NTT during this period, the ESO Imaging Survey (EIS). To obtain an insight into the efficiency of service observing, we examined the Period 60 NTT observing logs in detail. We have only compared nighttime operations, and do not include pre-observing preparations into our analysis. The observations in Service Mode suffered significantly more from adverse weather conditions at La Silla than both the VIS and EIS observations. On average, the down time during Service Mode (both weather and technical down time) is more than double the down time during either the VIS and EIS Mode, 23.7% versus 10.9% and 10.4% respectively. Irrespective of these adverse weather conditions during Service Mode, it can be

ISAAC at the VLT.

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ISAAC sees first light at the VLT.

ISAAC at the VLT.