Wine and Cheese Spring 2016 - Revision history

Gailzasowski at 14:43, 25 April 2016

2016-04-25T14:43:27Z

← Older revision		Revision as of 14:43, 25 April 2016
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	'''Radiative Hydrodynamics Simulations of IR and UV Radiative Pressure on Dusty AGN Tori''' <br>		'''Radiative Hydrodynamics Simulations of IR and UV Radiative Pressure on Dusty AGN Tori''' <br>
	Substantial evidence points to dusty, geometrically thick tori obscuring the central engines of AGNs, but so far no mechanism satisfactorily explains why cool dust in the torus remains in a puffy geometry. IR radiation pressure on dust can play a significant role in shaping the torus, yet the separation of hydrodynamic evolution from radiative transfer in previous work on radiation-supported tori precluded a self-consistent picture. Here we present the first three-dimensional radiative hydrodynamics simulations of dusty AGN tori subject to point-source UV and diffuse IR radiative acceleration. We discuss the implications of our results on torus morphology and dynamics, as well as the possible role the torus plays in galactic feedback.		Substantial evidence points to dusty, geometrically thick tori obscuring the central engines of AGNs, but so far no mechanism satisfactorily explains why cool dust in the torus remains in a puffy geometry. IR radiation pressure on dust can play a significant role in shaping the torus, yet the separation of hydrodynamic evolution from radiative transfer in previous work on radiation-supported tori precluded a self-consistent picture. Here we present the first three-dimensional radiative hydrodynamics simulations of dusty AGN tori subject to point-source UV and diffuse IR radiative acceleration. We discuss the implications of our results on torus morphology and dynamics, as well as the possible role the torus plays in galactic feedback.

	~~=April 25th=~~
	~~==Name==~~
	~~'''Title''' <br>~~
	~~Abstract~~

	~~=May 2nd=~~
	~~==Name==~~
	~~'''Title''' <br>~~
	~~Abstract~~

Gailzasowski: /* Chi Ho Chan */

2016-04-13T18:37:30Z

Chi Ho Chan

← Older revision		Revision as of 18:37, 13 April 2016
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	==Chi Ho Chan==		==Chi Ho Chan==
	'''~~Self-consistent radiative hydrodynamics simulations~~ of ~~dusty~~ AGN Tori''' <br>		'''Radiative Hydrodynamics Simulations of IR and UV Radiative Pressure on Dusty AGN Tori''' <br>
	~~TBD~~		Substantial evidence points to dusty, geometrically thick tori obscuring the central engines of AGNs, but so far no mechanism satisfactorily explains why cool dust in the torus remains in a puffy geometry. IR radiation pressure on dust can play a significant role in shaping the torus, yet the separation of hydrodynamic evolution from radiative transfer in previous work on radiation-supported tori precluded a self-consistent picture. Here we present the first three-dimensional radiative hydrodynamics simulations of dusty AGN tori subject to point-source UV and diffuse IR radiative acceleration. We discuss the implications of our results on torus morphology and dynamics, as well as the possible role the torus plays in galactic feedback.

	=April 25th=		=April 25th=

Kdkuntz: /* Leo Singer */

2016-04-11T13:16:03Z

Leo Singer

← Older revision		Revision as of 13:16, 11 April 2016
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	=April 11th=		=April 11th=
	==Leo Singer==		==Leo Singer==
	'''~~Title~~''' <br>		'''Advanced LIGO First Light: Astrophysics with a Gravitational-Wave Observatory''' <br>
	~~Abstract~~		Advanced LIGO's direct observation of gravitational radiation from a binary black hole merger has sent quakes through the physics and astronomy community, not to mention popular culture. In a few short years, the search for gravitational waves will complete its transformation from an experimental effort into a new discipline of observational astronomy as we rapidly build a sample of merging compact binaries. However, the greatest prize of all may come from combining our new GW observatories with existing electromagnetic ones---uncovering the host environments and formation channels of compact binaries, explaining the cosmic inventory of r-process elements, and even testing if stellar-mass black hole binaries are truly barren of matter or magnetic fields. I will describe the LIGO/Virgo EM follow-up program in detail. It brings together groundbreaking real-time GW data analysis techniques, a score of on-duty GW astronomers, and 63 groups who are searching for counterparts of LIGO sources using ground- and space-based partner facilities spanning gamma ray, x-ray, optical, infrared, and radio wavelengths. During LIGO's first observing run, these facilities embarked upon heroic broadband observing campaigns of LIGO/Virgo triggers including GW150914. In recounting this campaign, I will focus especially on my own role in leading follow-up with the Palomar Transient Factory. I will then describe how our GW analyses, human vetting, and follow-up consortium should evolve in the coming months to cope with an anticipated detection every few weeks by O2 and O3. I will introduce some ideas for the future to leverage GW distance estimates, large scale cosmography, and targeted infrared follow-up to measure the host properties of GW events, both with and without an electromagnetic counterpart.

	=April 18th=		=April 18th=

Gailzasowski: /* Joel Green */

2016-04-04T18:31:36Z

Joel Green

← Older revision		Revision as of 18:31, 4 April 2016
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	=April 18th=		=April 18th=
	==Joel Green==		==Joel Green==
	'''~~Title~~''' <br>		'''Anatomy of a Burst: The Evolution of FU Orionis Disks''' <br>
	~~Abstract~~		Most low mass young stars accrete at modest rates that gradually diminish as the system evolves, the circumstellar envelope thins, and the accretion disk accretes onto the central star, agglomerates in disk regions, or forms protoplanetary objects. FU Orionis objects (FUors, named after the class archetype) offer a potential counterpoint to the recent discovery of the “Luminosity Problem”, the observation that most nearby protostars are underluminous compared with models of core formation in molecular clouds. The rare dramatic outbursts of FUors, in which their accretion rates increase up to a thousandfold for short (10–100 yr) bursts, could account for the missing mass accretion if they represent a stage that all protostars occupy for a small fraction of their lifetime. These bursts also will modify the protoplanetary disk chemistry and require a very different model than simple magnetospheric accretion. Modern telescopes can track these bursts in progress when they occur, to address key questions: (1) what triggers a burst and what are the lasting effects on circumstellar disks and (2) are FUor bursts common to all stars? And did it happen here?

	==Chi Ho Chan==		==Chi Ho Chan==
	'''Self-consistent radiative hydrodynamics simulations of dusty AGN Tori''' <br>		'''Self-consistent radiative hydrodynamics simulations of dusty AGN Tori''' <br>

Ajmendez at 14:50, 30 March 2016

2016-03-30T14:50:36Z

← Older revision		Revision as of 14:50, 30 March 2016
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	=April 11th=		=April 11th=
	==~~Name~~==		==Leo Singer==
	'''Title''' <br>		'''Title''' <br>
	Abstract		Abstract

Tlan at 14:42, 25 March 2016

2016-03-25T14:42:13Z

← Older revision		Revision as of 14:42, 25 March 2016
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	==Zhilei Xu==		==Zhilei Xu==
	'''~~Title~~''' <br>		'''Measuring CMB polarization with Cosmology Large Angular Scale Surveyor (CLASS)''' <br>
	~~Abstract~~		During the past decades, CMB temperature anisotropy measurement brought cosmology to a precision era, strongly supporting the 6-parameter LCDM model. However, hints beyond LCDM emerged with increasingly precise measurements.While not much more information still remains in CMB temperature anisotropy and CMB polarization anisotropy provides another rich source of information, the polarization measurement is the crucial way to boost our understanding on our universe. In my talk, I will first talk about the standing issues (say cosmic inflation, parameter degeneracy and neutrino mass etc.) from current CMB anisotropy measurement and how they can be solved by CMB polarization anisotropy measurement, especially at large angular scales. Then I will introduce our in-house project CLASS which was uniquely designed to answer these questions. At last, I will give an update on the deployment of our first telescope in Chile.

Tlan at 00:32, 22 March 2016

2016-03-22T00:32:58Z

← Older revision		Revision as of 00:32, 22 March 2016
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	=March 28th=		=March 28th=
	==Ravi Sankrit==		==Ravi Sankrit==
	'''~~Title~~''' <br>		'''The Stratospheric Observatory for Infrared Astronomy (SOFIA)''' <br>
	~~Abstract~~		SOFIA is an airborne observatory, with a 2.7 meter telescope mounted on board a Boeing 747SP aircraft. SOFIA operates at altitudes of up to 45,000 feet, above 99% of the water vapor in the Earth's atmosphere, and provides access to the mid and far-infrared wavelength regions, which are not available from ground-based observatories.

			The observing programs undertaken by SOFIA are driven by peer-reviewed General Investigator proposals from the world-wide astronomy community. SOFIA started its 4th annual cycle of observations in February 2016; the Cycle 5 Call for Proposals is scheduled for release at the end of April 2016.

			In this talk, I will describe the observatory, the instruments and their capabilities, present some of the exciting science accomplished using SOFIA, give an overview of the proposal process, and conclude with a brief look ahead to the future of the mission.

	==Zhilei Xu==		==Zhilei Xu==

Ajmendez: /* Max Gronke */

2016-03-04T21:15:44Z

Max Gronke

@@ Line 65: / Line 65: @@
 Stellar streams in the Milky Way are unique dynamical tracers of the dark matter halo, and provide strong tests of galaxy formation models. However, lack of proper motion data limits our understanding of stream orbits and dark halo properties. Thanks to the HST's excellent astrometric accuracy, we are now able to obtain high quality proper motions along stellar streams in the Milky Way. In this talk, I will present our results on HST projects for measuring proper motions along two stellar streams in the halo: the Sagittarius Stream and the Orphan Stream.
 == Max Gronke ==
-'''Title''' <br>
+'''Lyman-alpha observables of the high-z Universe''' <br>
-Abstract
+Lyman alpha (Lya) emission provides a unique window into the high
 =March 28th=

Ajmendez: /* Name */

2016-03-04T20:33:19Z

Name

← Older revision		Revision as of 20:33, 4 March 2016
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	'''HST Proper Motions along Stellar Streams: Constraining Dark Halo Properties of the Milky Way''' <br>		'''HST Proper Motions along Stellar Streams: Constraining Dark Halo Properties of the Milky Way''' <br>
	Stellar streams in the Milky Way are unique dynamical tracers of the dark matter halo, and provide strong tests of galaxy formation models. However, lack of proper motion data limits our understanding of stream orbits and dark halo properties. Thanks to the HST's excellent astrometric accuracy, we are now able to obtain high quality proper motions along stellar streams in the Milky Way. In this talk, I will present our results on HST projects for measuring proper motions along two stellar streams in the halo: the Sagittarius Stream and the Orphan Stream.		Stellar streams in the Milky Way are unique dynamical tracers of the dark matter halo, and provide strong tests of galaxy formation models. However, lack of proper motion data limits our understanding of stream orbits and dark halo properties. Thanks to the HST's excellent astrometric accuracy, we are now able to obtain high quality proper motions along stellar streams in the Milky Way. In this talk, I will present our results on HST projects for measuring proper motions along two stellar streams in the halo: the Sagittarius Stream and the Orphan Stream.
	==~~Name~~==		== Max Gronke ==
	'''Title''' <br>		'''Title''' <br>
	Abstract		Abstract

Tlan at 21:44, 2 March 2016

2016-03-02T21:44:28Z

← Older revision		Revision as of 21:44, 2 March 2016
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	'''Recovery of Large Angular Scale CMB Polarization for Instruments Employing Variable-delay Polarization Modulators		'''Recovery of Large Angular Scale CMB Polarization for Instruments Employing Variable-delay Polarization Modulators
	''' <br>		''' <br>
	~~Abstract~~		The Cosmology Large Angular Scale Surveyor (CLASS) will attempt to measure the inflationary CMB B-modes on the largest angular scales. In order to reach the largest scales from the ground, rapid polarization modulation is required. For CLASS, this will be done using a variable-delay polarization modulator (VPM). It is important to identify and mitigate any time-varying effects generated by the VPM. In this talk, I will go over the different time-varying effects that the VPM can introduce and discuss a strategy for removing these spurious signals from the data. I will show that systematic effects introduced by the VPM will not limit the sensitivity of CLASS.

	==Duncan Watts==		==Duncan Watts==