Wine and Cheese Fall 2014 - Revision history

Gz323 at 22:07, 23 December 2014

2014-12-23T22:07:31Z

← Older revision		Revision as of 22:07, 23 December 2014
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	This page records the schedule, titles and abstracts of the [[CAS_Wine_and_Cheese_Seminars\|JHU/STScI CAS Astrophysics Wine & Cheese Series]] in Fall 2014.		This page records the schedule, titles and abstracts of the [[CAS_Wine_and_Cheese_Seminars\|JHU/STScI CAS Astrophysics Wine & Cheese Series]] in Fall 2014.

	~~<br>~~

	<h2>[[CAS_Wine_and_Cheese_Seminars\|Back to W&C Schedule]] </h2>		<h2>[[CAS_Wine_and_Cheese_Seminars\|Back to W&C Schedule]] </h2>


	= Fall 2014 =		= Fall 2014 =

Gz323 at 22:07, 23 December 2014

2014-12-23T22:07:07Z

← Older revision		Revision as of 22:07, 23 December 2014
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	\|}		\|}

	<h2>[[CAS_Wine_and_Cheese_Seminars\|Back to W&C Schedule]]		This page records the schedule, titles and abstracts of the [[CAS_Wine_and_Cheese_Seminars\|JHU/STScI CAS Astrophysics Wine & Cheese Series]] in Fall 2014.

			<br>

			<h2>[[CAS_Wine_and_Cheese_Seminars\|Back to W&C Schedule]] </h2>


	= Fall 2014 =		= Fall 2014 =

Gz323: Moved Table to the abstract page.

2014-12-23T21:48:59Z

Moved Table to the abstract page.

← Older revision		Revision as of 21:48, 23 December 2014
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	<h2>[[CAS_Wine_and_Cheese_Seminars\|Back to W&C Schedule]]		<h2>[[CAS_Wine_and_Cheese_Seminars\|Back to W&C Schedule]]

			= Fall 2014 =

			{\| border="1" style="text-align:left;"
			! align="left" \|Date
			! Speaker
			! Title
			\|-
			\|-
			\|September 8 \|\| K.G. Lee (MPIA) \|\| [[Wine and Cheese Fall 2014#K. G. Lee\|The First z>2 Large-Scale Structure Map with Lyman-Alpha Forest Tomography from LBGs]]
			\|-
			\| \|\| Peter Behroozi (STScI) \|\| [[Wine and Cheese Fall 2014#Peter Behroozi\|Close Pairs: Observational Probes for how Halo Accretion Impacts Galaxy Star Formation]]
			\|-
			\|-
			\|September 15 \|\| Dheeraj Pasham (Maryland) \|\| [[Wine and Cheese Fall 2014#Dheeraj Pasham\|A 400 solar mass Black Hole Revealed while Mimicking a Stellar-mass Black Hole]]
			\|-
			\| \|\| Alexander Mendez (JHU) \|\| [[Wine and Cheese Fall 2014#Alex Mendez\|AEGIS+PRIMUS: The Clustering of X-ray, Mid-IR, and Radio-selected AGN]]
			\|-
			\|-
			\|September 22 \|\| Yacine Ali-Haïmoud (JHU) \|\| [[Wine and Cheese Fall 2014#Yacine Ali-Haïmoud\|Rotational spectroscopy of Interstellar PAHs]]
			\|-
			\| \|\| Jim Green (U. Colorado) \|\| [[Wine and Cheese Fall 2014#Jim Green\|Imaging in the FUSE Band: The Sub-Lyman alpha Explorer]]
			\|-
			\|-
			\|September 29 \|\| Remco van den Bosch (MPIA) \|\| [[Wine and Cheese Fall 2014#Remco van den Bosch\|Compact Galaxies and Super Massive Black Holes]]
			\|-
			\| \|\| Omer Bromberg (Princeton) \|\| [[Wine and Cheese Fall 2014#Omer Bromberg\|Can We Really Trust All That We Know on Short GRBs?]]
			\|-
			\|-
			\|October 6 \|\| Matthias Bartelmann (Univ. Heidelberg) \|\| [[Wine and Cheese Fall 2014#Matthias Bartelmann\|Joint Reconstruction of Galaxy Clusters from all Observables]]
			\|-
			\| \|\| Elizabeth Fernandez (KAI) \|\| [[Wine and Cheese Fall 2014#Elizabeth Fernandez\|The Science of Deduction: Interpreting Observations of the Epoch of Reionization]]
			\|-
			\|-
			\| October 13 \|\| Amy Reines (U Michigan) \|\| [[Wine and Cheese Fall 2014#Amy Reines\|Probing the Origin of Supermassive Black Holes with Dwarf Galaxies]]
			\|-
			\|-
			\| \|\| Nick Stone (Columbia) \|\| [[Wine and Cheese Fall 2014#Nick Stone\|Stellar Tidal Disruption: the Role of General Relativity]]
			\|-
			\|-
			\| October 20 \|\| Roseanne Cheng (JHU) \|\| [[Wine and Cheese Fall 2014#Roseanne Cheng\|Hydrodynamic Circularization of Stellar Tidal Disruption Debris]]
			\|-
			\|-
			\| \|\| Marcio Melendez (Maryland) \|\| [[Wine and Cheese Fall 2014#Marcio Melendez\|Herschel Far-infrared Photometry of the Swift Burst Alert Telescope Active Galactic Nuclei Sample of the Local Universe. I. PACS Observations]]
			\|-
			\|-
			\| October 27 \|\| Sarah Hoerst (JHU EPS) \|\| [[Wine and Cheese Fall 2014#Sarah Hoerst\|Haze Formation in Planetary Atmospheres: Lessons from the Lab]]
			\|-
			\|-
			\| \|\| Cora Uhlemann (LMU Munich) \|\| [[Wine and Cheese Fall 2014#Cora Uhlemann\|Large scale structure formation with the Schrödinger method]]
			\|-
			\|-
			\| November 3 \|\| Chun Ly (NASA Goddard) \|\| [[Wine and Cheese Fall 2014#Chun Ly\|Results from "Direct" Metallicity Studies of Metal-poor, Strongly Star-forming Galaxies]]
			\|-
			\|-
			\| \|\| Jeff Cummings (JHU) \|\| [[Wine and Cheese Fall 2014#Jeff Cummings\|The Initial-Final Mass Relation: Expanding Into Massive White Dwarfs]]
			\|-
			\|-
			\| November 10 \|\| Dominika Wylezalek (JHU) \|\| [[Wine and Cheese Fall 2014#Dominika Wylezalek\|The Large-scale Environments of Radio-loud AGN and Their Evolution across Cosmic Time]]
			\|-
			\|-
			\| \|\| Kevin Lewis (JHU EPS) \|\| [[Wine and Cheese Fall 2014#Kevin Lewis\|Orbital Dynamics and the Martian Rock Record]]
			\|-
			\|-
			\| November 17 \|\| Michael Kesden (UT Dallas) \|\| [[Wine and Cheese Fall 2014#Michael Kesden\|Effective Potentials and Morphological Transitions for Binary Black-hole Spin Precession]]
			\|-
			\|-
			\| \|\| Laura Blecha (Maryland) \|\| [[Wine and Cheese Fall 2014#Laura Blecha\|The Observability of Recoiling Black Holes as Offset Quasars]]
			\|-
			\|-
			\| November 24 \|\| Leonardo Almeida (JHU/São Paulo) \|\| [[Wine and Cheese Fall 2014#Leonardo Almeida\|O-type binaries in 30 Doradus: Spectroscopic orbits, fundamental parameters, and distance to this region]]
			\|-
			\|-
			\| \|\| Anastasia Fialkov (ICFP, Paris) \|\| [[Wine and Cheese Fall 2014#Anastasia Fialkov\|The Rich Complexity of 21-cm Fluctuations Produced by the First Stars]]
			\|-
			\|-
			\| December 1 \|\| Hsiang-Yi Karen Yang (Maryland) \|\| [[Wine and Cheese Fall 2014#Hsiang-Yi Karen Yang\|The Fermi Bubbles: Possible Nearby Laboratory for AGN Jet Activity]]
			\|-
			\|-
			\| \|\| Sjoert van Velzen (JHU) \|\| [[Wine and Cheese Fall 2014#Sjoert van Velzen\|Jets from Supermassive Black Holes: from Giants to Newborns]]
			\|-
			\|-
			\| December 8 \|\| Richard Anderson (JHU) \|\| [[Wine and Cheese Fall 2014#Richard Anderson\|Cepheid radial velocity curve modulation impacts Baade-Wesselink distances]]
			\|-
			\|-
			\| \|\| Karrie Gilbert (STScI) \|\| [[Wine and Cheese Fall 2014#Karrie Gilbert\|The Global Properties of M31’s Stellar Halo: Results from the SPLASH Survey]]
			\|-
			\|-
			\| December 15 \|\| Yicheng Guo (UCSC) \|\| [[Wine and Cheese Fall 2014#Yicheng Guo\|The formation and evolution of clumpy galaxies from z=3 to z=0.5]]
			\|-
			\|-
			\| \|\| Amaya Moro-Martin (STScI) \|\| [[Wine and Cheese Fall 2014#Amaya Moro-Martin\|Herschel studies of extrasolar Kuiper belt-like systems]]
			\|-
			\|-
			\|}


	= 8 Sept 2014 =		= 8 Sept 2014 =

Gailzasowski: /* Amaya Moro-Martin */

2014-12-04T17:10:25Z

Amaya Moro-Martin

← Older revision		Revision as of 17:10, 4 December 2014
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	== Amaya Moro-Martin ==		== Amaya Moro-Martin ==
	'''~~Title~~''' <br>		'''Herschel studies of extrasolar Kuiper belt-like systems''' <br>
	~~Abstract~~
			Planetesimals are the building blocks of planets. They can be traced by the dust they produce in collisions or sublimation that forms a debris disk. In the solar system, such a dust disk is produced by the asteroids, comets and Kuiper Belt objects, with a dust production rate that has changed significantly with time, being higher in the past when the planetesimal belts were more densely populated. The Herschel DEBRIS, DUNES, and GT programs observed 37 extrasolar planetary systems within 25 pc. With a sensitivity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the current solar system’s Kuiper belt, these surveys identified 11 debris disks, indicating the presence of planetesimals. We discuss the general characteristics of these Kuiper belt-like disks and the correlations between the stellar, planetary, and debris components. We also present results from an unbiased subsample of the Herschel surveys consisting of 204 FGK stars, located at distances <20 pc, with ages > 100 Myr, and with no binary companions at <100 AU, and discuss whether the presence of planets affect the frequency and properties of extrasolar Kuiper belts. Is there evidence that debris disks are more common, or more dusty, or have a different characteristic temperature around stars harboring high-mass or low-mass planets compared to a control sample without identified planets? Are debris disks more or less common, or more or less dusty, around stars harboring multiple planets compared to single-planet systems? The study of extrasolar Kuiper belt-like disks can shed light on planet formation and migration scenarios. It can also help assess whether terrestrial planet detection might be feasible in these systems. The debris dust can cause an important observational issue for direct detection, with the level of zodiacal light being one of the parameters that defines the design of future telescopes like ATLAST, that have a goal of detecting biosignatures. From our unbiased subsample, we find that 14% of solar-type stars harbor dust-producing planetesimals at 10s of AU from the star with a distribution of fractional luminosity (L_dust/L_star) that can be reproduced by a Gaussian centered at the solar-system’s level. A Gaussian distribution centered at 10× the solar-system’s value can be ruled out. Because this dust would drift into the terrestrial planet region under PR drag, this indicates that there are good prospects for finding a large number of debris-disk systems—with evidence of harboring planetesimals—with zodi emission low enough to be appropriate targets for terrestrial-planet searches.

Gailzasowski: /* Speaker */

2014-12-04T17:01:09Z

Speaker

← Older revision		Revision as of 17:01, 4 December 2014
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	A common feature of star-forming galaxies at z>1 is the existence of giantstar-forming clumps,which are fundamental to our understanding of the accretionhistory of galaxies, formation of bulges, and evolution of gas-rich disks. Inthis talk, I will present our work on linking high-redshift clumpy galaxies andlow-redshift settled (rotation dominated) disks in three aspects: (1) thephysical properties of high-redshift clumps; (2) the evolution of the fractionof clumpy galaxies from z=3 to z=0.5; and (3) the connection between the clumpyappearance and the kinematics of settled and unsettled disks at z~0.5. Thethree aspects provide important clues of tracing the physical mechanisms thatare responsible for transferring distant clumpy galaxies into disk galaxies seen in the local universe.		A common feature of star-forming galaxies at z>1 is the existence of giantstar-forming clumps,which are fundamental to our understanding of the accretionhistory of galaxies, formation of bulges, and evolution of gas-rich disks. Inthis talk, I will present our work on linking high-redshift clumpy galaxies andlow-redshift settled (rotation dominated) disks in three aspects: (1) thephysical properties of high-redshift clumps; (2) the evolution of the fractionof clumpy galaxies from z=3 to z=0.5; and (3) the connection between the clumpyappearance and the kinematics of settled and unsettled disks at z~0.5. Thethree aspects provide important clues of tracing the physical mechanisms thatare responsible for transferring distant clumpy galaxies into disk galaxies seen in the local universe.

	== ~~Speaker~~ ==		== Amaya Moro-Martin ==
	'''Title''' <br>		'''Title''' <br>
	Abstract		Abstract

Hotaka: /* Karrie Gilbert */

2014-12-03T15:52:04Z

Karrie Gilbert

← Older revision		Revision as of 15:52, 3 December 2014
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	== Karrie Gilbert ==		== Karrie Gilbert ==
	'''~~Title~~''' <br>		'''The Global Properties of M31’s Stellar Halo: Results from the SPLASH Survey''' <br>
	~~Abstract~~		Large surveys of Andromeda's resolved stellar populations have revolutionized our view of this galaxy over the past decade. The combination of large-scale, contiguous photometric surveys and pointed spectroscopic surveys has been particularly powerful for discovering and following up new substructures and disentangling the structural components of Andromeda. The SPLASH survey has now amassed spectra of nearly ten thousand of red giant branch stars in Andromeda's halo, disk, and dwarf galaxies. I will present recent results from the SPLASH survey, focusing on the spatial structure and metallicity gradient of M31’s halo.

	= 15 Dec 2014 =		= 15 Dec 2014 =

Gailzasowski: /* Richard Anderson */

2014-12-03T14:11:43Z

Richard Anderson

← Older revision		Revision as of 14:11, 3 December 2014
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	== Richard Anderson ==		== Richard Anderson ==
	'''Cepheid radial velocity curve modulation impacts Baade-Wesselink distances''' <br>		'''Cepheid radial velocity curve modulation impacts Baade-Wesselink distances''' <br>
	Classical Cepheids are ~~excellent~~ distance tracers ~~that~~ carry high weight in the determination of the Hubble parameter ~~and~~ are ~~thus crucial for the extragalactic distance scale~~ and ~~cosmology~~. The Baade-Wesselink technique ~~is unique in its ability to determine~~ precise distances to individual Cepheids in both the Milky Way and the Magellanic Clouds and is ~~therefore~~ essential for investigating how metallicity affects the famous Cepheid period-luminosity relation. Here, I will present the recent discovery of ~~modulated~~ Cepheid radial velocity curves and show that modulation leads to a new, previously ignored, systematic uncertainty for Baade-Wesselink distances. In the worst case, modulation can lead to systematic distance errors as high as 15%. However, modulation may also ~~hold~~ the key for improving the precision of Baade-Wesselink distances.		Classical Cepheids are crucial Galactic and extragalactic distance tracers thanks to the famous period-luminosity relation and carry high weight in the determination of the Hubble parameter. Precise individual Cepheid distances are required to accurately calibrate this relation and in particular its zero-point. The Baade-Wesselink technique enables the determination of precise distances to individual Cepheids in both the Milky Way and the Magellanic Clouds and is thus essential for investigating how metallicity affects the famous Cepheid period-luminosity relation. Here, I will present the recent discovery of modulation in Cepheid radial velocity curves and show that modulation leads to a new, previously ignored, systematic uncertainty for Baade-Wesselink distances. In the worst case, modulation can lead to systematic distance errors as high as 15%. However, modulation may also be the key for improving the precision of Baade-Wesselink distances.

	== Karrie Gilbert ==		== Karrie Gilbert ==

Hotaka: /* Richard Anderson */

2014-12-03T03:35:29Z

Richard Anderson

← Older revision		Revision as of 03:35, 3 December 2014
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	= 8 Dec 2014 =		= 8 Dec 2014 =
	== Richard Anderson ==		== Richard Anderson ==
	'''~~Title~~''' <br>		'''Cepheid radial velocity curve modulation impacts Baade-Wesselink distances''' <br>
	~~Abstract~~		Classical Cepheids are excellent distance tracers that carry high weight in the determination of the Hubble parameter and are thus crucial for the extragalactic distance scale and cosmology. The Baade-Wesselink technique is unique in its ability to determine precise distances to individual Cepheids in both the Milky Way and the Magellanic Clouds and is therefore essential for investigating how metallicity affects the famous Cepheid period-luminosity relation. Here, I will present the recent discovery of modulated Cepheid radial velocity curves and show that modulation leads to a new, previously ignored, systematic uncertainty for Baade-Wesselink distances. In the worst case, modulation can lead to systematic distance errors as high as 15%. However, modulation may also hold the key for improving the precision of Baade-Wesselink distances.

	== Karrie Gilbert ==		== Karrie Gilbert ==
	'''Title''' <br>		'''Title''' <br>

Gz323: /* 15 Dec 2014 */ Added Yicheng

2014-11-21T21:56:53Z

15 Dec 2014: Added Yicheng

← Older revision		Revision as of 21:56, 21 November 2014
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	= 15 Dec 2014 =		= 15 Dec 2014 =
	== Yicheng Guo ==		== Yicheng Guo ==
			'''The formation and evolution of clumpy galaxies from z=3 to z=0.5''' <br>

			A common feature of star-forming galaxies at z>1 is the existence of giantstar-forming clumps,which are fundamental to our understanding of the accretionhistory of galaxies, formation of bulges, and evolution of gas-rich disks. Inthis talk, I will present our work on linking high-redshift clumpy galaxies andlow-redshift settled (rotation dominated) disks in three aspects: (1) thephysical properties of high-redshift clumps; (2) the evolution of the fractionof clumpy galaxies from z=3 to z=0.5; and (3) the connection between the clumpyappearance and the kinematics of settled and unsettled disks at z~0.5. Thethree aspects provide important clues of tracing the physical mechanisms thatare responsible for transferring distant clumpy galaxies into disk galaxies seen in the local universe.

			== Speaker ==
	'''Title''' <br>		'''Title''' <br>
	Abstract		Abstract

Gz323: /* 1 Dec 2014 */ Added Sjoert

2014-11-20T22:16:03Z

1 Dec 2014: Added Sjoert

← Older revision		Revision as of 22:16, 20 November 2014
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	== Sjoert van Velzen ==		== Sjoert van Velzen ==
	'''''' <br>		'''Jets from Supermassive Black Holes: from Giants to Newborns''' <br>
	~~Abstract~~
			Why do only 10% of quasar show powerful radio jets? The answer to this question is currently unknown but should involve at least one fundamental property of supermassive black holes (eg, spin or mass) as well as the evolution of their host galaxies. This talk, I will approach the questions of radio loudness from two different angles. First, using the lobes of radio galaxies to study jets on long (> million year) timescales. Second, using the tidal disruption of stars by massive black holes to probe jets on human timescales.

	= 8 Dec 2014 =		= 8 Dec 2014 =