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  • TAMU Galaxies Group
    environments form stars assemble mass and produce other observed relations in modern clusters Brett Salmon My research is studying the SFR mass relation at high redshift via SED fitting of photometric redshifts I examine physical properties from the posterior probability distribution such as UV luminosity and Mass evolution I also study the impact of nebular emission lines on broadband photometry and Lyman Break Galaxies in CANDELS GOODS S ERS UDF Paola Oliva Whitman Howard Uploading Images Uploads through the web ui don t work because we don t have write access to the web server So to upload images to your page you ll have to use sftp to upload the images to the file server io physics tamu edu using your physics ID and password Place your images into a folder with your name in the home websites galaxies physics tamu edu htdocs images directory To put the image into a page simply put the whole url to the image with img tags For example img size 120 https galaxies physics tamu edu images example jpeg img Alteratively if you do not have write access to the galaxy page images directory you can create a folder called public html

    Original URL path: https://galaxies.physics.tamu.edu/index.php/Main_Page (2014-11-01)
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  • Jimmy - TAMU Galaxies Group
    the galaxies are strongly rotating with λ Re as high as 0 5 Galaxies Being Studied Here s the list in no particular order of Target BCGs analyzed Clicking on a BCG will bring you to a page showing results for that galaxy The galaxies from the 2nd data set have a star by them to mark them as new 1027 1042 1048 1050 1066 1067 1153 1261 2001 2039 2086 Figures Mostly the kind that would be included in a paper λ R Vs Plots λ R Vs Radius Angular momentum profile Our sample of galaxies are plotted with thick orange and green lines The SAURON sample is plotted in grey Fast rotators are plotted as solid lines and slow rotators are plotted as dashed lines Fast rotators have a convex profile and slow rotators have a concave profile λ Re Vs Ellipticity λ at the effective radius as a function of ellipticity SAURON galaxies are plotted as triangles ATLAS 3D galaxies are plotted as crosses BCGs from this study are plotted as squares and Companion galaxies from this study are plotted as plus symbols The blue line indicates the division between fast rotating and slow rotating galaxies We find that four BCGs 1027 1048 1153 1261 and four companions 1027 1066 1048 are classified as fast rotators λ Re Vs Mass Angular momentum parameter λ Re versus dynamical mass M dyn Galaxies in this study orange and green are compared to the SAURON sample grey The galaxies presented here are amongst the most massive studied In the SAURON data set λ Re decreases with mass where as we see little correlation in our data set Everything Plot Merger status and angular momentum at the effective radius BCGs are plotted as squares and companions are plotted as crosses Plot

    Original URL path: https://galaxies.physics.tamu.edu/index.php/Jimmy (2014-11-01)
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  • Adam Tomczak - TAMU Galaxies Group
    where we have identified multiple candidate clusters as overdensities of sources with red Spitzer IRAC colors from Papovich 2008 Our NEWFIRM imaging includes three medium band J1 J2 J3 and two broad band H Ks filters and is 80 complete at 21 3 AB in Ks Combined with existing CFHTLS optical imaging ugriz we achieve photometric redshifts accurate to a few percent as these bands track the 4000 Angstrom Balmer break through redshifts 1 3 z 2 0 Currently our analysis of these data show three likely associations of galaxies from 1 3 z 2 0 We present properties of these three galaxy overdensities including color magnitude and color radius relations which support the idea that they are progenitors of present day massive galaxy clusters Z FOURGE Z FOURGE is a large scale near IR survey using the FOURSTAR instrument The primary motivation of this project is to study galaxy evolution at z 1 Several high z galaxy clusters have already been targeted My goal is to contribute to the data reduction of these targets as well as any following data analysis Extras Playground Retrieved from https galaxies physics tamu edu index php title Adam Tomczak oldid 967 Navigation menu

    Original URL path: https://galaxies.physics.tamu.edu/index.php/Adam_Tomczak (2014-11-01)
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  • Brett Salmon - TAMU Galaxies Group
    to upload figures LBG Candidate Selection Lake Burley Griffin is an artificial lake in the centre of Canberra the capital of Australia Lloyds Banking Group is a major British financial institution Little Babooshka s Grind is a rock group from Chennai India Retrieved from https galaxies physics tamu edu index php title Brett Salmon oldid 145 Navigation menu Personal tools Log in create account Namespaces Page Discussion Variants Views Read

    Original URL path: https://galaxies.physics.tamu.edu/index.php/Brett_Salmon (2014-11-01)
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  • Paola Oliva - TAMU Galaxies Group
    and the array that contains the percentages of light that each annuli will cover I does not remove the back ground automatically therefore the way to identify the effective radius is through the kinematics informations Once you have clear how far the effective radius gets you can look for the suitable annuli by testing the key is to find the best signal to noise configuration The code goes as fallow 1 Selects the respective spaxels for each annuli Using the kinematic information 2 Corrects by velocities 3 Picks a reference velocity dispersions and convolves each spectra to sigma ref 4 Stacks the spaxels Results one spectrum per annuli with a given signal to noise z 0 and sigma ref Code to extract stellar populations out of the spectra STECKMAP STECKMAP is a whole spectrum fitting code takes only one spectrum at the time and is written in Yorick The codes measures light weighted stellar populations and metallicities as well as the kinematics roughly Errors can be calculated be the MCMC of the code Using MILES stellar population library The command I use for each spectrum is Yorick command line Lick Indices Science After several preliminary tests these are the first fairly accurate results The signal to noise of the spectra span from 20 to 70 the average is 45 The errors are the standard deviation of 40 MCMC realisations Age and metallicity gradients The galaxies are classified according to Naabs 13 They show 5 different evolutionary path in the following plots I put together the ones that have gone through several major mergers class E late poor Mj SR class B late gas rich Mj FR only one or few major merger class C late rich Mj SR class D late poor Mj FR and the ones with only minor

    Original URL path: https://galaxies.physics.tamu.edu/index.php/Paola_Oliva (2014-11-01)
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  • Whitman Howard - TAMU Galaxies Group
    8 a uds v0 0 15 a cosmos v0 10 7 a Scripts Retrieved from https galaxies physics tamu edu index php title Whitman Howard oldid 1112 Navigation menu Personal tools Log in create account Namespaces Page Discussion Variants Views Read View source View history Actions Search Navigation Main page Jimmy s Page Adam Tomczak s Page Brett Salmon s Page Recent changes Help Tools What links here Related changes

    Original URL path: https://galaxies.physics.tamu.edu/index.php/Whitman_Howard (2014-11-01)
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  • TAMU Galaxies Group
    My goal is help provide insight into how galaxies in these environments form stars assemble mass and produce other observed relations in modern clusters Brett Salmon My research is studying the SFR mass relation at high redshift via SED fitting of photometric redshifts I examine physical properties from the posterior probability distribution such as UV luminosity and Mass evolution I also study the impact of nebular emission lines on broadband photometry and Lyman Break Galaxies in CANDELS GOODS S ERS UDF Paola Oliva Whitman Howard Uploading Images Uploads through the web ui don t work because we don t have write access to the web server So to upload images to your page you ll have to use sftp to upload the images to the file server io physics tamu edu using your physics ID and password Place your images into a folder with your name in the home websites galaxies physics tamu edu htdocs images directory To put the image into a page simply put the whole url to the image with img tags For example img size 120 https galaxies physics tamu edu images example jpeg img Alteratively if you do not have write access to the galaxy

    Original URL path: https://galaxies.physics.tamu.edu/index.php?title=Main_Page&oldid=1092 (2014-11-01)
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  • Log in - TAMU Galaxies Group
    logging in Retrieved from https galaxies physics tamu edu index php Special UserLogin Navigation menu Personal tools 213 175 86 38 Talk for this IP address Log in create account Namespaces Special page Variants Views Actions Search Navigation Main page

    Original URL path: https://galaxies.physics.tamu.edu/index.php?title=Special:UserLogin&returnto=Main+Page (2014-11-01)
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