Wine and Cheese Spring 2015 - Revision history

Tlan at 14:54, 21 July 2015

2015-07-21T14:54:48Z

← Older revision		Revision as of 14:54, 21 July 2015
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	<h2>[[CAS_Wine_and_Cheese_Seminars\|Back to W&C Schedule]] </h2>		<h2>[[CAS_Wine_and_Cheese_Seminars\|Back to W&C Schedule]] </h2>



			== [[Wine and Cheese Spring 2015\|Spring 2015 Schedule]] ==

			{\| border="1" style="text-align:left;"
			! align="left" \|Date
			! Speaker
			! Title
			\|-
			\|-
			\|January 26 \|\| Ingyin Zaw (NYU Abu Dhabi) \|\| [[Wine and Cheese Spring 2015#Ingyin Zaw\|Probing the Central Parsec of Active Galactic Nuclei with Water Masers]]
			\|-
			\| \|\| Naoki Bessho (NASA/UMD) \|\| [[Wine and Cheese Spring 2015#Naoki Bessho\|Particle acceleration during magnetic reconnection in ultrarelativistic electron-positron plasmas]]
			\|-
			\|-
			\|February 02 \|\| Marius Millea (UC Davis) \|\| [[Wine and Cheese Spring 2015#Marius Millea\|Planck 2015 Constraints on the Cosmic Neutrino(-like) Background]]
			\|-
			\| \|\| Colin Hill (Columbia) \|\| [[Wine and Cheese Spring 2015#Colin Hill\|Cosmology from the One-Point Function]]
			\|-
			\|-
			\|February 09 \|\| Katherine Lee (Harvard) \|\| [[Wine and Cheese Spring 2015#Katherine Lee\|CARMA Large Area Star Formation Survey (CLASSy)]]
			\|-
			\| \|\| Rongmon Bordoloi (STScI) \|\| [[Wine and Cheese Spring 2015#Rongmon Bordoloi\|Investigating the Milky Way’s Nuclear Outflow Kinematics]]
			\|-
			\|-
			\|February 16 \|\| Yacine Ali-Haïmoud (JHU) \|\| [[Wine and Cheese Spring 2015#Yacine Ali-Haïmoud\|Perturbative interaction approach to cosmological structure formation]]
			\|-
			\| \|\| Nao Suzuki (IPMU) \|\| [[Wine and Cheese Spring 2015#Nao Suzuki\|Future SNIa surveys and Blackbody Spectra]]
			\|-
			\|-
			\|February 23 \|\| Rubab Khan (GSFC) \|\| [[Wine and Cheese Spring 2015#Rubab Khan\|Massive Star Geriatrics]]
			\|-
			\| \|\| Jon Bird (Vanderbilt) \|\| [[Wine and Cheese Spring 2015#Jon Bird\|Clues to Galaxy Formation from the Milky Way's Cosmological Context]]
			\|-
			\|-
			\|March 02 \|\| Alexie Leauthaud (IPMU, Full seminar) \|\| [[Wine and Cheese Spring 2015#Alexie Leauthaud\|Evolving Galaxies in a Dark Universe]]
			\|-
			\|-
			\|-
			\|-
			\| March 09 \|\| Nicole Czakon (ASIAA) \|\| [[Wine and Cheese Spring 2015#Nicole Czakon\|Scaling Sunyaev-Zel'dovich Observables to Dark Matter Halos for Cluster Cosmology ]]
			\|-
			\|-
			\| \|\| Kate Daniel (JHU) \|\| [[Wine and Cheese Spring 2015#Kate Daniel\|Constraints on the Efficiency of Radial Migration in Spiral Galaxies]]
			\|-
			\|-
			\| March 23 \|\| Kendrick Smith (Perimeter) \|\| [[Wine and Cheese Spring 2015#Kendrick Smith\|Primordial Non-Gaussianity in the CMB and Large-Scale Structure]]
			\|-
			\|-
			\| \|\| Sanch Borthakur (JHU) \|\| [[Wine and Cheese Spring 2015#Sanch Borthakur\|Probing the Connection Between the Circumgalactic Medium and the Interstellar Medium of Galaxies]]
			\|-
			\|-
			\| March 30 \|\| Katie Harrington (JHU) \|\| [[Wine and Cheese Spring 2015#Katie Harrington\|CLASS: The Cosmology Large Angular Scale Surveyor]]
			\|-
			\|-
			\| \|\| Peter Polko (UMD) \|\| [[Wine and Cheese Spring 2015#Peter Polko\|From Accretion Flow to Particle Acceleration: New Relativistic Magnetohydrodynamic Jet Solutions]]
			\|-
			\|-
			\| April 06 \|\| Tomohiro Nakama \|\| [[Wine and Cheese Spring 2015#Tomohiro Nakama\|On whether supermassive black holes can be explained by primordial black holes]]
			\|-
			\|-
			\| \|\| Brooks Kinch (JHU) \|\| [[Wine and Cheese Spring 2015#Brooks Kinch\|Fe K-alpha Emission Lines from Simulations of Black Hole Accretion]]
			\|-
			\|-
			\| April 13 \|\| Xavier Dumusque (CfA) \|\| [[Wine and Cheese Spring 2015#Xavier Dumusque\|Pushing the radial-velocity precision to unveil Earth-mass exoplanets]]
			\|-
			\|-
			\| \|\| Samantha Hoffmann (JHU) \|\| [[Wine and Cheese Spring 2015#Samantha Hoffmann\|Mega-SH0ES: Searching for Cepheid Variables in Type Ia Supernova Host Galaxies]]
			\|-
			\|-
			\| April 20 \|\| Liang Dai (JHU) \|\| [[Wine and Cheese Spring 2015#Liang Dai\|Relativistic clustering and separate universes]]
			\|-
			\|-
			\| \|\| Jennifer Sobeck (UVa) \|\| [[Wine and Cheese Spring 2015#Jennifer Sobeck\|APOGEE I/O: Efforts to Effectively Harness the Large Scale Data Set of the APOGEE 1+2 Survey]]
			\|-
			\|-
			\| April 27 \|\| Johan Mazoyer (STScI) \|\| [[Wine and Cheese Spring 2015#Johan Mazoyer\|Extrasolar Planetary Systems Imaging]]
			\|-
			\|-
			\| \|\| Daan Meerburg (CITA) \|\| [[Wine and Cheese Spring 2015#Daan Meerburg\|Optimal estimator for resonant bispectra in the Cosmic Microwave Background]]
			\|-
			\|-
			\| May 04 \|\| Agnieszka Cieplak (Brookhaven National Laboratory) \|\| [[Wine and Cheese Spring 2015#Agnieszka Cieplak\|Theoretical Predictions of Large Scale Clustering in the Lyman-alpha Forest]]
			\|-
			\|-
			\| \|\| Lixin Dai (UMD) \|\| [[Wine and Cheese Spring 2015#Lixin Dai\|X-ray Temperature Tidal Disruption Events from Stars on Deep Plunging Orbits]]
			\|-
			\|-
			\| May 11 \|\| Tim Brandt (IAS) \|\| [[Wine and Cheese Spring 2015#Tim Brandt\|Extended Main Sequence Turnoffs in ~1-1.5 Gyr-old Clusters: Age Ranges or Stellar Rotation?]]
			\|-
			\|-
			\| \|\| Alvise Raccanelli \|\| [[Wine and Cheese Spring 2015#Alvise Raccanelli\|Testing cosmological models with galaxy surveys]]
			\|-
			\|-
			\|}

Tlan at 23:09, 7 May 2015

2015-05-07T23:09:32Z

← Older revision		Revision as of 23:09, 7 May 2015
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	to probe		to probe
	the angular momentum distribution and evolution of stars at low metallicity.		the angular momentum distribution and evolution of stars at low metallicity.

			==Alvise Raccanelli==
			'''Testing cosmological models with galaxy surveys'''<br>
			The strangest feature of our current cosmological model is the observation that the expansion rate of the universe is accelerating. Our ignorance is summarized by the simple name for the cause of the observed phenomenon: dark energy. Alternatively, it could be explained by the break down of Einstein's gravitation theory on cosmological scales. Observations of large-scale structure have played an important role in developing our standard cosmological model and will play an essential role in our investigations of the origin of cosmic acceleration.
			However, the theoretical models currently used to interpret the data often rely on simplifications that make them not accurate enough for precise measurements at very large scales.
			I will show improvements to the theoretical modeling that arise when using a proper general relativistic formalism, and illustrate how it is possible to test different models of gravity, dark matter, dark energy and inflation via galaxy clustering using forthcoming cosmological galaxy surveys.

Tlan: /* Tim Brandt (IAS) */

2015-05-07T00:15:00Z

Tim Brandt (IAS)

← Older revision		Revision as of 00:15, 7 May 2015
Line 161:		Line 161:
	= 11 May 2015 =		= 11 May 2015 =

	== Tim Brandt ~~(IAS)~~ ==		== Tim Brandt ==
	'''Extended Main Sequence Turnoffs in ~1-1.5 Gyr-old Clusters: Age Ranges or Stellar Rotation?''' <br>		'''Extended Main Sequence Turnoffs in ~1-1.5 Gyr-old Clusters: Age Ranges or Stellar Rotation?''' <br>
	Stellar evolution models have failed to reproduce the main sequence		Stellar evolution models have failed to reproduce the main sequence

Tlan: /* Tim Brandt */

2015-05-07T00:14:40Z

Tim Brandt

@@ Line 162: / Line 162: @@
 == Tim Brandt (IAS) ==
-'''TBD''' <br>
+'''Extended Main Sequence Turnoffs in ~1-1.5 Gyr-old Clusters: Age Ranges or Stellar Rotation?''' <br>
-TBD
+Stellar evolution models have failed to reproduce the main sequence

Tlan: /* Lixin Dai (UMD) */

2015-04-30T13:36:10Z

Lixin Dai (UMD)

← Older revision		Revision as of 13:36, 30 April 2015
Line 155:		Line 155:
	With the recent progress of Lyman-alpha forest power spectrum measurements, understanding of the bias between the measured flux and the underlying matter power spectrum is becoming crucial to the percent level cosmological interpretation of these measurements. Whereas previous theoretical studies of this bias have used N-body and hydro-PM simulations, we have run hydrodynamic simulations to study the response of the Lyman-alpha forest clustering to large wavelength modes of the underlying matter large-scale structure. Our results demonstrate that this can be simulated by evolving smaller, curved universe cosmologies, representing the same universe with different overdense patches. We use these to study the assumptions of the analytical bias formula derived by Seljak (2012), and compare these results with previous numerical methods of determining bias. With several forthcoming large data sets, such theoretical predictions are important to fully understand the clustering of the Lyman-alpha forest and its cosmological implications.		With the recent progress of Lyman-alpha forest power spectrum measurements, understanding of the bias between the measured flux and the underlying matter power spectrum is becoming crucial to the percent level cosmological interpretation of these measurements. Whereas previous theoretical studies of this bias have used N-body and hydro-PM simulations, we have run hydrodynamic simulations to study the response of the Lyman-alpha forest clustering to large wavelength modes of the underlying matter large-scale structure. Our results demonstrate that this can be simulated by evolving smaller, curved universe cosmologies, representing the same universe with different overdense patches. We use these to study the assumptions of the analytical bias formula derived by Seljak (2012), and compare these results with previous numerical methods of determining bias. With several forthcoming large data sets, such theoretical predictions are important to fully understand the clustering of the Lyman-alpha forest and its cosmological implications.

	== Lixin Dai ~~(UMD)~~ ==		== Lixin Dai ==
	'''X-ray Temperature Tidal Disruption Events from Stars on Deep Plunging Orbits''' <br>		'''X-ray Temperature Tidal Disruption Events from Stars on Deep Plunging Orbits''' <br>
	When a star approaches a supermassive black hole closer than its tidal radius, the star can be deformed and disrupted by the black hole tidal field. Such events can be used to probe quiescent supermassive black holes and help us understand accretion/jet physics around black holes. The canonical picture by Rees 1988 predicts that in such events a small accretion disk forms from stellar debris and the light curve follows the mass fallback rate. However, recent hydrodynamical simulations have shown that this picture, especially the fast circularization of debris, cannot be easily realized. It is then quite puzzling why some observed TDEs have light curves following the fallback rate and have spectra peaked at soft X-ray temperature. In this talk we will employ first-order calculations to show that such X-ray temperature TDEs can be produced from stars disrupted on orbits with high penetration parameters.		When a star approaches a supermassive black hole closer than its tidal radius, the star can be deformed and disrupted by the black hole tidal field. Such events can be used to probe quiescent supermassive black holes and help us understand accretion/jet physics around black holes. The canonical picture by Rees 1988 predicts that in such events a small accretion disk forms from stellar debris and the light curve follows the mass fallback rate. However, recent hydrodynamical simulations have shown that this picture, especially the fast circularization of debris, cannot be easily realized. It is then quite puzzling why some observed TDEs have light curves following the fallback rate and have spectra peaked at soft X-ray temperature. In this talk we will employ first-order calculations to show that such X-ray temperature TDEs can be produced from stars disrupted on orbits with high penetration parameters.

Tlan at 13:33, 30 April 2015

2015-04-30T13:33:55Z

← Older revision		Revision as of 13:33, 30 April 2015
Line 156:		Line 156:

	== Lixin Dai (UMD) ==		== Lixin Dai (UMD) ==
	'''~~TBD~~''' <br>		'''X-ray Temperature Tidal Disruption Events from Stars on Deep Plunging Orbits''' <br>
	~~TBD~~		When a star approaches a supermassive black hole closer than its tidal radius, the star can be deformed and disrupted by the black hole tidal field. Such events can be used to probe quiescent supermassive black holes and help us understand accretion/jet physics around black holes. The canonical picture by Rees 1988 predicts that in such events a small accretion disk forms from stellar debris and the light curve follows the mass fallback rate. However, recent hydrodynamical simulations have shown that this picture, especially the fast circularization of debris, cannot be easily realized. It is then quite puzzling why some observed TDEs have light curves following the fallback rate and have spectra peaked at soft X-ray temperature. In this talk we will employ first-order calculations to show that such X-ray temperature TDEs can be produced from stars disrupted on orbits with high penetration parameters.

	= 11 May 2015 =		= 11 May 2015 =

Hotaka: /* Agnieszka Cieplak */

2015-04-29T00:15:46Z

Agnieszka Cieplak

← Older revision		Revision as of 00:15, 29 April 2015
Line 152:		Line 152:

	== Agnieszka Cieplak ==		== Agnieszka Cieplak ==
	'''~~TBD~~''' <br>		'''Theoretical Predictions of Large Scale Clustering in the Lyman-alpha Forest''' <br>
	~~TBD~~		With the recent progress of Lyman-alpha forest power spectrum measurements, understanding of the bias between the measured flux and the underlying matter power spectrum is becoming crucial to the percent level cosmological interpretation of these measurements. Whereas previous theoretical studies of this bias have used N-body and hydro-PM simulations, we have run hydrodynamic simulations to study the response of the Lyman-alpha forest clustering to large wavelength modes of the underlying matter large-scale structure. Our results demonstrate that this can be simulated by evolving smaller, curved universe cosmologies, representing the same universe with different overdense patches. We use these to study the assumptions of the analytical bias formula derived by Seljak (2012), and compare these results with previous numerical methods of determining bias. With several forthcoming large data sets, such theoretical predictions are important to fully understand the clustering of the Lyman-alpha forest and its cosmological implications.

	== Lixin Dai (UMD) ==		== Lixin Dai (UMD) ==
	'''TBD''' <br>		'''TBD''' <br>

Gz323: /* 27 April 2015 */

2015-04-27T17:44:00Z

27 April 2015

← Older revision		Revision as of 17:44, 27 April 2015
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	= 27 April 2015 =		= 27 April 2015 =

	== ~~Laurent Pueyo~~ ==		== Johan Mazoyer ==

	'''~~TBD~~''' <br>		'''Extrasolar Planetary Systems Imaging''' <br>
	~~TBD~~		Johan will discuss the development of innovative instruments for imaging circumstellar environments and in the analysis of high contrast images to detect and analyze planets and/or dust at close separations around these stars.

	== Daan Meerburg ==		== Daan Meerburg ==

Tlan at 18:56, 22 April 2015

2015-04-22T18:56:36Z

← Older revision		Revision as of 18:56, 22 April 2015
Line 146:		Line 146:
	== Daan Meerburg ==		== Daan Meerburg ==

	'''~~TBD~~''' <br>		'''Optimal estimator for resonant bispectra in the Cosmic Microwave Background''' <br>
	~~TBD~~		With a cosmic variance limited measurement of the CMB power spectrum we have almost exhausted the information available in the almost Gaussian CMB. Within the next years we hope to further explore the polarization and measure higher order correlation functions in the CMB that improve our understanding of the early Universe. In this talk I will focus on a particular class of CMB bispectra known as resonant bispectra. These spectra have rapidly varying features on top of the late-time BOA features. Only recently, and only for a limited number of frequencies, have these bispectra been constrained using the Planck data. I will discuss a newly proposed estimator of such bispectra and show that we should be able to probe any frequency that one expect from an EFT argument (and beyond), because the estimator relies on the fact that most of the theoretical shapes are at most 1 dimensional (while the full bispectrum is 3 dimensional).

	= 04 May 2015 =		= 04 May 2015 =

Gailzasowski: /* Jennifer Sobeck */

2015-04-17T14:21:13Z

Jennifer Sobeck

← Older revision		Revision as of 14:21, 17 April 2015
Line 134:		Line 134:

	== Jennifer Sobeck ==		== Jennifer Sobeck ==
	'''~~TBD~~''' <br>		'''APOGEE I/O: Efforts to Effectively Harness the Large Scale Data Set of the APOGEE 1+2 Survey''' <br>
	~~TBD~~		The first phase of the Apache Point Observatory Galactic Evolution Experiment (APOGEE-1), a cornerstone project of the Sloan Digital Sky Survey III (SDSS-III), performed a large-scale, spectroscopic survey of the Milky Way conducted from the Northern Hemisphere, aimed at tracing the chemodynamical evolution of the Milky Way. Now, the SDSS-IV APOGEE-2 Survey is underway, with observations being carried out at both Northern and Southern Hemisphere locations. APOGEE acquires high-resolution, high signal-to-noise spectra in the H-band (1.51-1.69 microns) and produces stellar atmospheric parameters, individual element abundance ratios for 15 species, and radial velocity measurements for its stars. By 2020, data will have been collected for several hundred thousand stars from all components of the Galaxy (all disk quadrants, the inner and outer halo, the full expanse of the bulge, and local satellites). Accordingly, the combined APOGEE 1+2 data set is tailor-made for the comprehensive and systematic examination of Galactic formation and evolution. I will give an updated overview of the APOGEE 1+2 Survey, briefly discuss endeavors to improve the data product determination (such as enhancing the atomic physics inputs), and describe initial data mining efforts and the use of APOGEE data products to assemble composite chemical and kinematic profiles for target stellar populations.

	= 27 April 2015 =		= 27 April 2015 =