Seminars 8 gas laws


Abstract:I will provide a brief history of the new field of exoplanetology, from its birth in 1995 to the present. The initial discovery of 51 Peg b posed a mystery: how can giant planets be present extremely close to their parent star? The field has evolved since with a number of issues and new surprises. electricity usage calculator south africa From the study of giant planets, their sizes, compositions, the field moved towards smaller planets. A number of close-in planets between the mass of Neptune and that of the Earth were discovered, often in highly compact configurations. Understanding how they were formed is among the most active area in this field. We are now entering the epoch of exoplanet characterisation, i.e., the spectra of some exoplanets can now be acquired, their atmospheric dynamics can be studied. In parallel, this led to a race to discover the most favorable targets. The study of exoplanets and their parent star(s) opens a new window to understand our Universe.

earlier in summer. We are now finding a young SNe ( 0.4. Emission lines of [OII]3727, Hb, [OIII]4959,5007, Ha, [NII]6549,6584 and [SII]6717,6731 have been measured to study the ionized gas properties in the SNR candidates. Our analysis with SITELLE confirmed, with optical spectroscopy, the shock-excited nature of these sources. The question of the optimal background subtraction will be presented.

Abstract:ZFOURGE and ZFIRE are deep observational surveys that track how galaxies assemble over cosmic time. ZFOURGE identifies approximately 70,000 objects up to redshifts of z~7 using a custom set of near-infrared imaging filters that provide high precision photometric redshifts. electricity 101 video ZFIRE selects galaxies from ZFOURGE for spectroscopic follow-up to measure how baryons cycle between stars, winds, and the Inter-Stellar Medium (ISM) at z~2. Here I highlight results that include building a library of composite Spectral Energy Distributions and properties of galaxies in clusters at z~2.

Abstract: The study of the evolution of quasars and their influence on their host galaxies provides unique insight into how supermassive black holes became a ubiquitous feature of galaxies today. Dust-reddened quasars appear to represent a transitional phase in merger-driven models of quasar/galaxy co-evolution. I will present results from recent and ongoing surveys to identify these transitional systems using infrared and radio selection. The results of these surveys reveal that red quasars are among the most intrinsically-luminous quasars in the Universe, and make up ~20% of the overall quasar population. They reside in actively merging galaxies, and their rest-frame UV spectra exhibit outflows in absorption and emission. electricity word search pdf I will discuss how reddened quasars fit into the larger picture of AGN evolution which includes both mergers and secular growth. Finally, I will present new work on surveys to explore red-quasars’ parameter space to fully understand the connection between galaxy mergers and black hole growth.

Abstract: The ESA Euclid space mission core science goals rely on complementary deep ground-based surveys covering both the northern and southern galactic caps. This talk will present an overview of the space survey design and the current status of the ground-based survey campaign, with a focus on its forerunner, CFHT’s Canada-France Imaging Survey.

Abstract: Devasthal Optical Telescope Integral Field Spectrograph (DOTIFS) is a new multi-Integral Field Unit (IFU) instrument being designed and fabricated by the Inter-University Center for Astronomy and Astrophysics (IUCAA), Pune, India, for the Cassegrain side port of the 3.6m Devasthal Optical Telescope, operated by the Aryabhatta Research Institute of Observational Sciences (ARIES). The science drivers mainly focus on nearby galaxies, which are the primary targets of the instrument. This includes star formation and kinematics of nearby galaxies, galactic HII regions, merging and interacting galaxies, etc. DOTIFS has sixteen IFUs, which can be deployed over an 8 arcminute diameter telescope focal plane. Each IFU sees 8.7 arcsec x 7.4 arcsec on the sky and is composed of a 12 x 12 array of hexagonal shape microlenses each of which is 0.8 arcsec vertex to vertex. Optical fibers are attached to the back side of each microlens to gather and transfer light to the spectrographs. Eight identical, all refractive, dedicated spectrographs cover 2,304 fibers, with 288 fibers (from two IFUs) per spectrograph. electricity in india Its wavelength coverage is 370-740nm, and the spectral resolution is 1200 – 2400 over the wavelength range. In this talk, I will present an overview and current development status of the instrument.

Abstract: The universe has provided us with multiplanet systems, laboratories in which we can test the physics of planet formation. I will talk about three ways in which we can use multiplanet systems as laboratories. (1) We can study the orbital dynamics of a single multi-planet system in detail. (2) In each multiplanet system, we can compare a planet to its siblings, developing statistics over many systems. (3) We can compare multiplanet systems to systems with only one known planet. My talk will draw on results from the California Kepler Survey, which provided new stellar and planetary properties for 909 transiting planets in 355 multiplanet systems, as well as recent dynamical work.

Abstract:Stellar mass black holes (a few tens of Msun) resulting from end-stage stellar evolution and supermassive black holes (10^6 – 10^9) found in the cores of most galaxies are well established in the observational literature. What are conspicuously absent are detections of black holes with mass between these two extremes. Intermediate mass black holes (IMBHs) in the range of 10^3 – 10^5 Msun have yet to be conclusively discovered, but their proposed formation mechanisms imply that the dense stellar environments in the cores of globular clusters are a good place to look for them.

Our study searches for the kinematic signature of an IMBH in the core of the globular cluster 47 Tucanae. We utilize ultraviolet HST photometry to produce proper motion data for ~50,000 stars in the cluster core. By comparing the velocity dispersions profile of the cluster to theoretical Jeans-derived models and N-body simulations, we detect the influence of a modestly-sized IMBH. Our current estimate for the IMBH mass is something like 2500 +/- 1000 Msun, though our model is undergoing continuous adjustment.

Abstract:Massive stars strongly influence their immediate surroundings during their lifetimes (via e.g. protostellar jets, strong stellar winds, ionising radiation, supernovae). On larger scales, feedback from massive stars regulates the formation and evolution of entire stellar clusters and dominates the mass and energy cycle in star-forming galaxies like the Milky Way. Qualitatively, the effect of massive stars on their environment is well understood, but a solid quantitative, observational analysis is still missing. The results of recent feedback observations of a variety of structures and environments within massive star-forming regions will be shown, carried out with the integral field spectrographs MUSE and KMOS at the Very Large Telescope. I will discuss the advantages (and caveats) of integral field spectroscopy in tracing and quantifying feedback from massive stars, and describe the bigger picture that connects feedback on small (cloud) scales to that on large (galactic) scales.

Abstract:Observations of the dynamics of stars and gas in the nuclear regions of nearby galaxies suggest that the overwhelming majority of spheroidal galaxies in the local Universe contain massive black-holes (BH) and that, with some important caveats, the masses of those central BH correlate with the velocity dispersion of the stars in the spheroid and the bulge luminosities. 3 gas laws Much research has been dedicated to understanding the mechanisms responsible for such a fundamental – perhaps causal – relation. An accurate census of the basic properties of the cold interstellar medium (ISM) in galaxies with accreting super-massive black holes at their centers, i.e. galaxies that host active galactic nuclei (AGN), is pertinent to those investigations because cold molecular gas fuels both black hole growth and star-formation.

We present high sensitivity observations taken with the Herschel Space Observatory to estimate the cold ISM content in a sample of ~200 nearby,optically luminous QSOs. The cold ISM properties of these luminous AGN are discussed in the context of models that envision that quasar activity is triggered by gas-rich galaxy mergers. We also present infrared spectroscopic and photometric observations of a sample of ~200 nearby, Luminous Infrared Galaxies (LIRGs). Luminous Infrared Galaxies (LIRGs) make stars and grow super-massive black holes (SMBH) at a faster rate than most of their local counterparts. electricity in costa rica current Their number density increase with redshift until z~1 when they dominate galaxy evolution. Some are mergers, some are not, some are feeding the central SMBH, others may not be. Because of this, LIRGS constitute a perfect laboratory to observe and study how galaxies grow and to test the conditions in which gas rich mergers trigger episodes of growth for the central SMBH and the host galaxy.

Abstract:The Solo (Solitary Local) Dwarf Galaxy Survey is a volume limited sample of all nearby ( 300 kpc from the Milky Way or M31) dwarfs, with wide-field g and i imaging. This survey uses resolved stellar populations to parameterize these low mass systems. Comparison to the well studied satellite dwarfs characterizes the evolutionary impact of a large galaxy in close proximtity. The deep, wide field nature of this survey also lends itself to searching for substructure around these dwarfs, both globular clusters and possible faint satellites. I present a subset of Solo dwarfs, which lie within the virial radius of the Local Group. This sample has been characterized using consistent methods, despite their diversity in mass and size. The analysis focuses on extended faint stellar structure, stellar populations and morphology. gas news in hindi We intend to use this subset to examine trends with star formation history, and separation from a large host. This first subset emphasizes both the unique challenges and advantages of this survey. The Solo Survey provides detailed look at the extended structure of dwarfs and helps to characterize the evolution of galaxies in the faint limit.

The past three years have witnessed a revolution in microlensing searches for exoplanets. Spitzer campaigns in 2014, 2015, and 2016 have transformed space-based microlensing observations from a novelty to an industry. Campaign 9 of Kepler’s extended K2 mission conducted the first automated microlensing survey from the ground and from space. These endeavors facilitate measuring a key observable known as the satellite parallax, which leads to model-independent mass measurements for the lensing systems and opens a new window for astrophysical exploration. I will discuss the scientific methodology and utility of these missions, highlight several key results, and emphasize the preparatory work for and expected yields of the WFIRST microlensing survey.