http://hayne.net/MacDev/Notes/unixFAQ.html#shellStartup
http://secrets.blacktree.com/
Sunday, July 22, 2012
Thursday, July 19, 2012
Sunday, July 15, 2012
http://www.makeuseof.com/pages/best-mac-apps
Author: Date Written: Title: Subject Area: Source Website: ---Summary--- ---My Reaction--- ---Questions---
Friday, July 13, 2012
The Merger Environment of the Wide Agle Tail Hosting Cluster A562
Author: Douglass, Blaton, et. al.
Date Written: December 20, 2011
Title: The Merger Environment of the Wide Agle Tail Hosting Cluster A562
Subject Area: Galaxies, Active galaxies, clusters, A562 galaxy, intracluster medium, galaxies in X-rays
Source Website:
---Notes---
physical environment studied: galaxy cluster
units: cgs and mks
WAT's are high power raadio sources generally associated with the bright central galaxy at or enar the center of its host cluster.
a562 is a galaxy cluster.
CIAO was used for data reduction
WAT radio sources
VLA radio data in 1.4 and 8.4 GHz range
Flux calibrations were done. What does '3c48 ' was 'use as a flux calibrator' mean?
Optical data from Perkins and the PRISM instrument was used.
3.
Adaptively smoothe? Background was subtracted using an observation specifc exposure map.
How was exposure subtracted?
---Summary---
Results: constrained interal desntiy of jets and plasma flow velocity with the lobes of the Wide Angle Tail (WAT) soruce
---
figure 3, the X-ray and radio data does not seem related to each other
3. 1
ram pressure?
3.2
the cluster was fit with a beta 2d model in Sherpa4.2
Figure 4: what does it mean by SW? lower left? Shows surface brightness of two 65 degree wedges in image a, with surface brightness as a function of semi-major axis. This is semi major axis of a galaxy, as they are rotating within the cluster? I don't see an excess of brighness in the sW of the image
4: spectral analysis
Fit spectrum to ellipticall region centeredd on AGN with e=0.27 PA (position angle) = 60 degrees (?) Model was fit with APEC in XSPEC!
Spectral fit was done of the entire cluster and sections of the cluster broken up into ellipses with at least 1000 source counts
Lx- T plot?
--there is a lot of possible conclusions
-bolometric luminosity- total luminosity of all EM waves
Figure 9 , how is mass determined from spectra?
Does htis give 3-d information of X-ray surface brightness? a
routine that deprojects the X-ray surface brightness (see Blanton
et al. 2009) was used to give the emissivity as a function of
radius.
From wikipedia (Radio Galaxy), this is a common appearance of a radio galaxy, in this case 3C98.
So the line bisecting the WAT is perp. to the lobes I would think.
How is this conclusion made?
'''
A surface brightness profile was
extracted from a wedge of 30
due east of the cluster center
confirming the apparent edge (Figure 10). Such a feature is
likely an indication of a merger shock created by an infalling
subcluster from the east.
'''
Dont see the excess of emission in lower left of figure 4.
What is ICM flow velocity?
Many references to previous papers
Summary-
The galaxy cluster a562, which contains the merger-bent, WAT source 0647+693, was studied.
- X-ray images from Chandra showed relatively constant Temp as a function of radius, which indiates the absence of an active cooling flow.
-Surface brightness distrubion shows an elongation of the line which bisects the WAT, which is consistent with an ongoing merger ocuring parllel ot the line.
- 2-d temperature map shows a hot region just 'east' of the AGN, which likely is caused by merger induced shock heating.
- cluster image shows excess emission between the WAT lobes, which is likely gas displaced during an interaction.
-spectral analysis shows there is a high abundance of gas.
-time since core displacement
-Synchrotron lifetime
-combination of observational data with common merger values gives constraints on internal density of jets and plasma flow velocities within the lobes of the WAT.
---My Reaction---
---Questions---
Date Written: December 20, 2011
Title: The Merger Environment of the Wide Agle Tail Hosting Cluster A562
Subject Area: Galaxies, Active galaxies, clusters, A562 galaxy, intracluster medium, galaxies in X-rays
Source Website:
---Notes---
physical environment studied: galaxy cluster
units: cgs and mks
WAT's are high power raadio sources generally associated with the bright central galaxy at or enar the center of its host cluster.
a562 is a galaxy cluster.
CIAO was used for data reduction
WAT radio sources
VLA radio data in 1.4 and 8.4 GHz range
Flux calibrations were done. What does '3c48 ' was 'use as a flux calibrator' mean?
Optical data from Perkins and the PRISM instrument was used.
3.
Adaptively smoothe? Background was subtracted using an observation specifc exposure map.
How was exposure subtracted?
---Summary---
Results: constrained interal desntiy of jets and plasma flow velocity with the lobes of the Wide Angle Tail (WAT) soruce
---
figure 3, the X-ray and radio data does not seem related to each other
3. 1
ram pressure?
3.2
the cluster was fit with a beta 2d model in Sherpa4.2
Figure 4: what does it mean by SW? lower left? Shows surface brightness of two 65 degree wedges in image a, with surface brightness as a function of semi-major axis. This is semi major axis of a galaxy, as they are rotating within the cluster? I don't see an excess of brighness in the sW of the image
4: spectral analysis
Fit spectrum to ellipticall region centeredd on AGN with e=0.27 PA (position angle) = 60 degrees (?) Model was fit with APEC in XSPEC!
Spectral fit was done of the entire cluster and sections of the cluster broken up into ellipses with at least 1000 source counts
Lx- T plot?
--there is a lot of possible conclusions
-bolometric luminosity- total luminosity of all EM waves
Figure 9 , how is mass determined from spectra?
Does htis give 3-d information of X-ray surface brightness? a
routine that deprojects the X-ray surface brightness (see Blanton
et al. 2009) was used to give the emissivity as a function of
radius.
From wikipedia (Radio Galaxy), this is a common appearance of a radio galaxy, in this case 3C98.
So the line bisecting the WAT is perp. to the lobes I would think.
How is this conclusion made?
'''
A surface brightness profile was
extracted from a wedge of 30
due east of the cluster center
confirming the apparent edge (Figure 10). Such a feature is
likely an indication of a merger shock created by an infalling
subcluster from the east.
'''
Dont see the excess of emission in lower left of figure 4.
What is ICM flow velocity?
Many references to previous papers
Summary-
The galaxy cluster a562, which contains the merger-bent, WAT source 0647+693, was studied.
- X-ray images from Chandra showed relatively constant Temp as a function of radius, which indiates the absence of an active cooling flow.
-Surface brightness distrubion shows an elongation of the line which bisects the WAT, which is consistent with an ongoing merger ocuring parllel ot the line.
- 2-d temperature map shows a hot region just 'east' of the AGN, which likely is caused by merger induced shock heating.
- cluster image shows excess emission between the WAT lobes, which is likely gas displaced during an interaction.
-spectral analysis shows there is a high abundance of gas.
-time since core displacement
-Synchrotron lifetime
-combination of observational data with common merger values gives constraints on internal density of jets and plasma flow velocities within the lobes of the WAT.
---My Reaction---
---Questions---
Tuesday, July 10, 2012
Wednesday, July 4, 2012
scientific writing links
http://www.astro.caltech.edu/~lah/ay31/
http://physics.illinois.edu/people/Celia/SciWrite.pdf
http://www.elsevier.com/wps/find/journaldescription.cws_home/601274/authorinstructions
http://rmp.aps.org/files/rmpguapa.pdf
UW astro 482 page
http://aas.org/career
http://www.astro.washington.edu/groups/outreach/tjo/
http://aas.org/journals
http://www.journals.uchicago.edu/PASP/
http://authors.aps.org/
http://ksjtracker.mit.edu/
http://owl.english.purdue.edu/owl/
http://physics.illinois.edu/people/Celia/SciWrite.pdf
http://www.elsevier.com/wps/find/journaldescription.cws_home/601274/authorinstructions
http://rmp.aps.org/files/rmpguapa.pdf
UW astro 482 page
http://aas.org/career
http://www.astro.washington.edu/groups/outreach/tjo/
http://aas.org/journals
http://www.journals.uchicago.edu/PASP/
http://authors.aps.org/
http://ksjtracker.mit.edu/
http://owl.english.purdue.edu/owl/
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