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<channel>
	<title>sukye</title>
	<link>http://blogs.jhu.edu/sukye</link>
	<description>Where We Witness</description>
	<pubDate>Tue, 12 Aug 2008 04:35:48 +0000</pubDate>
	<generator>http://lyceum.ibiblio.org/?v=1.0.2</generator>
	<language>en</language>
			<item>
		<title>ghost file</title>
		<link>http://blogs.jhu.edu/sukye/2008/ghost-file/</link>
		<comments>http://blogs.jhu.edu/sukye/2008/ghost-file/#comments</comments>
		<pubDate>Tue, 03 Jun 2008 18:26:15 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2008/ghost-file/</guid>
		<description><![CDATA[FATAL ERROR:  Output Reference WCS &#8220;72_wcs.fits&#8221; already exists! Please delete.
&#8211;> delete 72_wcs.fits
Warning: Attempt to delete a nonexistent file (72_wcs.fits)
&#8212;&#8212;&#8212;
http://server.ccw.com.cn/yyjq/htm2005/20050906_0994b.htm
find . -name &#8220;graphcap&#8221; -print

]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2008/ghost-file/feed/</wfw:commentRss>
		</item>
		<item>
		<title>how to use tweakshifts</title>
		<link>http://blogs.jhu.edu/sukye/2008/how-to-use-tweakshifts/</link>
		<comments>http://blogs.jhu.edu/sukye/2008/how-to-use-tweakshifts/#comments</comments>
		<pubDate>Sat, 03 May 2008 19:20:59 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2008/how-to-use-tweakshifts/</guid>
		<description><![CDATA[we could register images precise to 0.1 pixel by iterating multidrizzle (mul) and tweakshifts (twe). since twe only works when the shifts are within 1 pixel or there are tiny rotations, we have to find the rough shifts by hand.
step 0.
create files list to be the input:
list_mul:
&#8212;&#8212;&#8212;&#8212;&#8212;-
a_flt.fits
b_flt.fits
&#8212;&#8212;&#8212;&#8212;&#8212;-
list_twe:
&#8212;&#8212;&#8212;&#8212;&#8212;-
a_single_sci.fits
b_single_sci.fits
&#8212;&#8212;&#8212;&#8212;&#8212;-
The first file will be the reference image.
step 1.
create [...]]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2008/how-to-use-tweakshifts/feed/</wfw:commentRss>
		</item>
		<item>
		<title>astro-ph 0802w1</title>
		<link>http://blogs.jhu.edu/sukye/2008/astro-ph-0802w1/</link>
		<comments>http://blogs.jhu.edu/sukye/2008/astro-ph-0802w1/#comments</comments>
		<pubDate>Mon, 04 Feb 2008 08:05:44 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2008/astro-ph-0802w1/</guid>
		<description><![CDATA[The Subaru/XMM-Newton Deep Survey (SXDS)
http://arxiv.org/abs/0801.4017
B=28.4, V=27.8, Rc=27.7, i&#8217;=27.7 and z&#8217;=26.6, 1.22 deg^2
Measuring the Fraction of Obscured Quasars by the Infrared Luminosity of Unobscured Quasars
http://arxiv.org/abs/0801.3849
collected archival 24 micron MIPS photometry from objects with z~1 in SDSS, GOODS, and COSMOS.
Although we find approximate agreement, our method indicates somewhat higher values of f_obsc, particularly in the middle range [...]]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2008/astro-ph-0802w1/feed/</wfw:commentRss>
		</item>
		<item>
		<title>astro-ph 0801w4</title>
		<link>http://blogs.jhu.edu/sukye/2008/astro-ph-0801w4/</link>
		<comments>http://blogs.jhu.edu/sukye/2008/astro-ph-0801w4/#comments</comments>
		<pubDate>Sun, 27 Jan 2008 23:26:54 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2008/astro-ph-0801w4/</guid>
		<description><![CDATA[NICMOS Measurements of the Near Infrared Background
http://arxiv.org/abs/0801.3825
he near infrared background is now spatially resolved and is dominated by galaxies in the redshift range between 0.5 and 1.5
Estimating the Redshift Distribution of Faint Galaxy Samples
http://arxiv.org/abs/0801.3822
assigns weights to galaxies in a spectroscopic subsample such that the weighted distributions of photometric observables (e.g., multi-band magnitudes) match the corresponding [...]]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2008/astro-ph-0801w4/feed/</wfw:commentRss>
		</item>
		<item>
		<title>astro-ph 0801w3</title>
		<link>http://blogs.jhu.edu/sukye/2008/astro-ph-0801w3/</link>
		<comments>http://blogs.jhu.edu/sukye/2008/astro-ph-0801w3/#comments</comments>
		<pubDate>Sun, 20 Jan 2008 12:32:43 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2008/astro-ph-0801w3/</guid>
		<description><![CDATA[http://arxiv.org/abs/0801.2759
Spitzer Uncovers AGN Missed by Optical Surveys in 7 Late-type Galaxies
Our findings add to the growing evidence that black holes do form and grow in low-bulge environments and that they are significantly more common than optical studies indicate.
http://arxiv.org/abs/0801.2694
Milli-arcsecond astrophysics with VSI, the VLTI spectro-imager in the ELT era
This instrument will provide information complementary to what [...]]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2008/astro-ph-0801w3/feed/</wfw:commentRss>
		</item>
		<item>
		<title>probability ABC</title>
		<link>http://blogs.jhu.edu/sukye/2008/probability-abc/</link>
		<comments>http://blogs.jhu.edu/sukye/2008/probability-abc/#comments</comments>
		<pubDate>Tue, 15 Jan 2008 00:53:12 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2008/probability-abc/</guid>
		<description><![CDATA[A priori probability is the probability estimate prior to receiving new information.
Posterior probability is a revised probability that takes into account new available information. For example, let there be two urns, urn A having 5 black balls and 10 red balls and urn B having 10 black balls and 5 red balls. Now if an [...]]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2008/probability-abc/feed/</wfw:commentRss>
		</item>
		<item>
		<title>Cosmology with Active Nuclei as Probes</title>
		<link>http://blogs.jhu.edu/sukye/2008/cosmology-with-active-nuclei-as-probes/</link>
		<comments>http://blogs.jhu.edu/sukye/2008/cosmology-with-active-nuclei-as-probes/#comments</comments>
		<pubDate>Tue, 08 Jan 2008 04:45:39 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2008/cosmology-with-active-nuclei-as-probes/</guid>
		<description><![CDATA[http://www.astr.ua.edu/keel/galaxies/qsoevolve.html
It has long been seductive to try probing the world model of cosmology by trying to use AGN as standard candles or standard measuring rods. Radio galaxies seen at 2.2 microns have a very well-behaved Hubble diagram, and for a while it appeared that radio QSOs with flat-spectrum core sources showed a neat relation between [...]]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2008/cosmology-with-active-nuclei-as-probes/feed/</wfw:commentRss>
		</item>
		<item>
		<title>constants</title>
		<link>http://blogs.jhu.edu/sukye/2007/constants/</link>
		<comments>http://blogs.jhu.edu/sukye/2007/constants/#comments</comments>
		<pubDate>Thu, 20 Dec 2007 13:21:03 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2007/constants/</guid>
		<description><![CDATA[pc = 3.1*10^(16) m = 3.26 ly
yr = 3.2*10^7 s
M_o = 2*10^(30) Kg
G = 20/3*10^(-11) Nm^2/Kg^2
10^0.4=2.5  10^0.6=4
Ln(10)=2.3
erg=10^(-7)J
tbc&#8230;

]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2007/constants/feed/</wfw:commentRss>
		</item>
		<item>
		<title>Particle sudoku</title>
		<link>http://blogs.jhu.edu/sukye/2007/particle-sudoku/</link>
		<comments>http://blogs.jhu.edu/sukye/2007/particle-sudoku/#comments</comments>
		<pubDate>Mon, 17 Dec 2007 09:25:34 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2007/particle-sudoku/</guid>
		<description><![CDATA[
top quark:
*only by the Tevatron at FermiLab, thousands per yr
*decay into bW in 10^-24 s, no time for meson or hadron
*170900 MeV, almost a gold atom
*since 1977, >8000 papers, now 300 per yr, >250 PhD
*LHC: millions per yr
]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2007/particle-sudoku/feed/</wfw:commentRss>
		</item>
		<item>
		<title>redshifted blackbody spectrum</title>
		<link>http://blogs.jhu.edu/sukye/2007/redshifted-blackbody-spectrum/</link>
		<comments>http://blogs.jhu.edu/sukye/2007/redshifted-blackbody-spectrum/#comments</comments>
		<pubDate>Thu, 06 Dec 2007 03:17:05 +0000</pubDate>
		<dc:creator>sukye</dc:creator>
		
		<category>Uncategorized</category>

		<guid isPermaLink="false">http://blogs.jhu.edu/sukye/2007/redshifted-blackbody-spectrum/</guid>
		<description><![CDATA[since the wavelengths are multiplied by a factor of (1+z), the spectrum at
temperature T &#038; redshift z will look like the blackbody spectrum at
temperature T/(1+z) with an additional factor (1+z)^5, or (1+z)^3
in the frequency diagram. 
12:00pm David J. Gross
15:30pm John C. Mather
]]></description>
		<wfw:commentRss>http://blogs.jhu.edu/sukye/2007/redshifted-blackbody-spectrum/feed/</wfw:commentRss>
		</item>
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