8/10 (7 votes) - Download OsiriX Mac Free. OsiriX is a DICOM viewer for macOS aimed at doctors and sanitary personnel. It's an image viewer for medical use backed by several different organizations. If you're a doctor that likes to make the most of new technologies, adapting them to your work. Cons: We are a Mac office, so the use of Parallels (to utilize Osiris with our Macs) with this PC based product has had it's challenges, but the Osiris staff has been with us every step of the way. That said, if your office uses Macs, I would still highly recommend Osiris.
Help can be found in the User's Guide which can be downloaded and is available in the OSIRIS program from the Help menu. Answers to questions and issues can also be found in the FAQ and Troubleshooting guide below, and in the User's Guide.
- Osiris is a beautiful game that uniquely combines inventive crafting, curious exploration, and skillful FPS combat gameplay that highlights the beauty and horror of exploring a foreign, yet gorgeous alien system - an experience that's neither safe nor for the timid.
- The dAppstore is completely integrated into the Osiris web browsing experience. Now it’s possible to use your favorite applications with all the benefits that the Decenternet promotes. Decenternet is a tech pioneer that utilizes blockchain technology to bring about decentralized, net.
Optimize OSIRIS
For the best performance using the latest improvements, OSIRIS settings must be optimized. Suggested starting analysis settings for either single source or mixed samples are available in the lab settings [PowerPlex Fusion HID Sole Source] and [GlobalFiler HID Mixture] in the OSIRIS program under the Tools > Lab Settings menu.
Updates
Subscribe now for announcements, new releases, and occasional updates.
Attention Mac users with OSIRIS version 2.12.1 and earlier - With newer versions of Mac OSX, sometimes the OSIRIS windows do not appear. This can be remedied by clicking on the OSIRIS icon in the dock (usually at the bottom of the screen) to activate the OSIRIS window. You may need to do this for each new window in OSIRIS. This issue should be resolved in OSIRIS versions 2.12.2 and later.
Topics
- Troubleshooting
Installing and upgrading OSIRIS
Attention Mac users with OSIRIS version 2.12.1 and earlier - With newer versions of Mac OSX, sometimes the OSIRIS windows do not appear. This can be remedied by clicking on the OSIRIS icon in the dock (usually at the bottom of the screen) to activate the OSIRIS window. You may need to do this for each new window in OSIRIS. This issue should be resolved in OSIRIS versions 2.12.2 and later.
While the other screen will control the screen one. So, you have control over the slides that you want to display others. Thus, using this approach you can make a better live presentation. Download propresenter 5 for mac.
When upgrading OSIRIS it is generally least confusing to remove old versions. On Windows, run the uninstall.bat file to uninstall MSI file installations, which will maintain your custom lab settings. Windows EXE or ZIP file installations may simply be deleted. Macintosh installations may simply be deleted. Remember to back up any custom lab settings before uninstalling. When installing multiple versions of OSIRIS for evaluation of newer versions, use EXE file installation on Windows. Use care to ensure that analyses are done with the correct version, when multiple versions are installed.
Contact Us
Questions and suggestions are welcome at .
FAQ
- Can I analyze .hid and .fsa file types?Yes. The Operating Procedure must be set for the appropriate file type. See General – .fsa and .hid files in Lab Settings.
- Can I enter a new kit in OSIRIS?Yes. See Appendix G for instructions. Contact us for help or advice.
- Can I use a different ILS?Several different ILS are defined for various kits. Note that some of those are actually one ILS, but use more or fewer of the peaks, in case not all peak data gets collected. If the ILS you use is not defined for the kit you use, see Appendix G for instructions on defining a new ILS. Contact us if you need help.
- What do I do if my multiplex has no ladder available?You can either construct a ladder, or you can use a DNA sizing ladder to add a new kit. See Appendix G or contact us for help.
- How fast is OSIRIS?OSIRIS should process 2 to 4 samples per second, depending on the number of artifacts in the samples and the speed of your computer/network. So a plate of 98 samples with controls should take 30-60 seconds to analyze. If it runs significantly slower than that on your system, contact us for advice.
- How many samples can OSIRIS process at once?OSIRIS will process at least 800 samples in a single batch (single directory). OSIRIS will process an essentially unlimited number of batches in a single processing run. This has been tested with approximately 10,000 samples in 110 directories (plates) in a single analysis that took approximately 1 hour 20 minutes.
- How many users can use OSIRIS at the same time?This is limited only by the number of client computers you have and the speed of your network and server. Generally, it should be “lots.” Additionally, each user is creating a separate instance of OSIRIS running on the local client, so multiple users will not affect the speed of operation except as limited by sample data flow across the network to and from the server if the sample data and OSIRIS output is being stored on the server. A single user can run separate instances of OSIRIS on the same computer at the same time (Windows only), allowing different analyses or tasks to be performed simultaneously. Multiple analyses can also be run from a single OSIRIS process (Windows and Macintosh).
- Is there any fee for OSIRIS software or use?No. OSIRIS is free and open source. No license or fees are required.
- Mac grapher for windows. Is OSIRIS source code available?Yes. OSIRIS source code is available at GitHub: https://github.com/ncbi/osiris.
- Can I modify OSIRIS, build it into my front end or incorporate it into my own software?OSIRIS is open source and public domain software. You may do anything your heart desires. In any work or product derived from this material, proper attribution to the authors as the source of the software would be appreciated.
Troubleshooting
Problems and Solutions
My analysis failed
- OSIRIS must have at least one acceptable ladder for the analysis to succeed. If the expected ILS or ladder allele peaks are below the analysis threshold or not present (e.g., cut off in collection) the ladder will fail to analyze. By opening a failed analysis, it may be possible to examine the ladder peaks to determine if the ladder was the reason the batch failed.
- A common cause of analysis failure is selection of the wrong kit or ILS definition in the Operating Procedure. Ensure that the correct kit and ILS combination is selected in the Operating Procedure being used for the analysis.
- Any time your analysis fails you can select the “Details” button to find troubleshooting information. Selecting “View Selection” or double clicking the failed run will open the ladder, if it could be found and partially analyzed. Click the ladder sample name to view all the channels of the ladder in the Preview pane or double click the ladder sample name to view it in the Graph View to determine the presence of artifacts and peaks and whether the locus and ILS peaks are below the analytical threshold.
- No ladder sample was present, or the file name did not contain the ladder file search string. OSIRIS requires a ladder for analysis.
- Artifact peaks made it impossible to analyze the ladder ILS. Sometimes this can be alleviated by adjusting the ILS analysis thresholds. Otherwise re-prepare or re-inject the ladder.
- The ladder’s ILS peaks are below threshold. Adjust the ILS analysis thresholds. Otherwise re-prepare or re-inject the ladder.
- The ladder’s allele peaks have artifacts or are below threshold. Sometimes this can be alleviated by adjusting the Ladder analysis thresholds. Otherwise re-prepare or re-inject the ladder.
My .hid/.fsa analysis failed
- If the Operating Procedure is not set for the correct file type on the General tab of the Lab Settings, the analysis will fail because no files of the expected type are present. If you select the failed run and click the details button, at the bottom of the list there will be a “Project did not meet expectations…No satisfactory ladder found…Ending” error message. Make sure that the correct file type is selected and reanalyze. Analysis of a directory tree with multiple file types will succeed only in those subfolders containing the expected file type.
I can’t edit the Operating Procedure
- To edit an Operating Procedure, you must have write permission to the site settings folder and its subfolders. To view this folder, select “Show site settings folder..” from the “Tools” menu on the menu bar.
- You cannot edit default Operating Procedures (shown in brackets) such as [PowerPlex 16]. Make a new Operating Procedure that can be edited.
- You cannot edit Operating Procedures opened through the “Parameters” button. These are static copies associated with the analysis file you are viewing. This is designed to preserve the history of the conditions used for a specific analysis.
- The Operating Procedure is locked while being edited by any user and cannot be edited by a second user or used for an analysis. Ask the user editing the Operating Procedure to close it or select a different OP.
- In Version 2.9.1 and earlier, locking the OP was based on the time it was last edited or used in an analysis:
Check to determine whether other users are editing or analyzing with that OP. If you try to edit the Operating Procedure immediately after your own analysis, it may still be locked. If you have just performed an analysis, wait 30 to 60 seconds and try again. Locking the OP prevents change in the middle of analysis, or corrupting the Operating Procedure if two users were to make changes at the same time. The “Lock” button at the lower left corner of the Lab Settings window will be active (not grayed out) if the Operating Procedure has been locked. When you can successfully click the Lock button, you may edit the settings. - If you are operating on a network or in a forensic or clinical laboratory, your OSIRIS administrator may have limited write permissions on the Operating Procedure directories to prevent unintended changes. Contact your OSIRIS administrator.
Text and notices do not display correctly on a Macintosh
- The OSIRIS display is not optimized for 'Dark Mode' on the Macintosh. Some text and notices do not display correctly when using Dark mode. To solve this issue, turn Dark mode off when using OSIRIS on the Macintosh.
Known issues
- 'Help' error: Some configurations of Microsoft Windows 10 will not open the OSIRIS Help document from within the program when the Microsoft Edge browser is the default reader for PDF files. This is a known MS Edge browser issue. The simplest solution is to select an alternate PDF reader: In File Explorer, open the folder where OSIRIS is installed. Right click the OsirisHelp.pdf file and select “Open with >” then “Choose another app” from the pop up context menu. Select a different PDF reader or a different browser that can open PDF files, check the “Always use this app to open .pdf files” checkbox, and click 'Ok'.
- Mac window issue: Mac users with OSIRIS version 2.12.1 and earlier and have newer versions of Mac OSX may find that the OSIRIS windows do not appear. This can be remedied by clicking on the OSIRIS icon in the dock (usually at the bottom of the screen) to activate the OSIRIS window. You may need to do this for each new window in OSIRIS. This issue should be resolved in OSIRIS versions 2.12.2 and later.
Privacy Information
Privacy Statement
but I don't want to pay the (EDIT: $400) to upgrade to 8GB RAM does that mean I will have to go with the 32-bit Windows 7 and 32-bit Inventor? Edited by: hcps-marsdenja on Apr 15, 2010 12:51 AM. I have Inventor 2011 running on 64-bit Win 7 on a mac book pro (1.5 years old), running 2.4 Ghz, 4 Gb ram, M9600GT graphics and 500Gb 7200 RPM drive. Inventor for mac autodesk. and running Inventor on Mac Bootcamp specifications: 'RAM: 3GB minimum Recommend 4GB for 32-bit guest OS, 8GB or more for 64-bit guest OS.'
OSIRIS is a desktop tool working on your computer with your own data. Your sample profile data is processed on your computer and is not sent over the internet.
For quality monitoring, OSIRIS versions 2.12 and higher send some information about usage statistics back to NCBI. This information is limited to use of the tool, without any sample, profile or batch data that would reveal the context of your analysis.
Opt-out of Statistics Collection
You can opt-out of statistics collection by performing the following operations:
- Open OSIRIS.
- Open the Tools menu and uncheck Allow Usage Reporting.
- OSIRIS will immediately stop reporting statistics.
See the OSIRIS User's Guide for additional details regarding usage statistics and opting out.
OSIRIS web pages
See the NCBI Privacy Policy for the policy that applies to the OSIRIS web pages.
![Osiris Osiris](https://static.giantbomb.com/uploads/square_small/6/63758/2342235-7002.sectoidfinal.jpg_610x0.jpg)
OSIRIS
OH-Suppressing Infra-Red Imaging SpectrographPI: James Larkin (UCLA) Project Scientist: Andreas Quirrenbach (UCSD) Co-PI: Alfred Krabbe (UC Berkeley) |
NOTE: The Keck OSIRIS Toolbox now has latest version of the OSIRIS pipeline.
Overview
OSIRIS is an integral field spectrograph designed to work with theKeck Adaptive Optics System. It uses an array of tiny lenses to samplea rectangular patch of the focal plane and produces spectra at up to3000 locations simultaneously. There is also an internal diffractionlimited camera with a 20x20 arcsec field of view. Both the camera andspectrograph can operate at wavelengths between 1 and 2.4 microns. Thecenter of the imaging camera’s field is about 20 arcsec offsetfrom the center of the spectrograph field and both can be usedsimultaneously with the same or different filters.
The spectrograph has plate scales of 0.02, 0.035, 0.05 and 0.10arcsec per lenslet. The spectral resolution averages 3800 in the threefinest plate scales, but is closer to 3400 in the 0.100 arcsec platescale. In the broadband mode each spectrum contains a full broad band(z, J, H or K) and a total of 16x64 (actually 1019) spectra aretaken. In the narrowband mode, a typical spectrum contains 1/4th of abroad band and an individual exposure contains between 16x64 to 48x64spectra depending on the exact filter selected. The imager has asingle fixed plate scale of 0.020 arcsec per pixel.
A great deal of thought has gone into trying to make OSIRIS easy touse. For the spectrograph, the only user selectable items are theplate scale, the filter, and the exposure time. The imager only has afilter and an exposure time setting. A great deal of complexity,however, is allowed in the observing sequences and the slaving of theimager to the spectrograph. All setup and control aspects of theinstrument are managed by a few GUIs.
There is also a data reduction system that includes a“real-time” reduction of raw frames into cubes for displayand basic analysis. In this real-time mode, it takes about one minutefor a preliminary data cube to appear in the “quicklook”display package. The reduction system also includes a growing set offinal reduction steps including correction of telluric absorption andmosaicing of multiple cubes.
First light was obtained on February 22, 2005 - See OSIRIS 1st Light Pictures!
The OSIRIS Toolbox
NOTE: Keck has become the primary distributor of the OSIRIS Data Reduction Pipeline. Some of the following information and files have been redirected to Keck! Please access the new OSIRIS Toolbox at this link: http://www2.keck.hawaii.edu/inst/osiris/tools/
The OSIRIS team and Keck staff would like to help OSIRIS users achieve a successful and rewarding observing experience! OSIRIS is an innovative and unique spectrograph, and hence it takes more preparation than traditional spectrographs with planning and reductions. We suggest looking over the OSIRIS manual prior to your observing run as well as the Keck OSIRIS webpage for further telescope and AO information. We have included links to the packages you will need for pre-observing (manual and planning GUI) and post-observing (Quicklook2 and data reduction pipeline).
OSIRIS User's Manual (pdf) - (v4.2 05/07/2018) Please refer to the OSIRIS manual for a complete description of OSIRIS capabilities, observational procedures, data reduction system, detector performance, filter curves, and much more.
OSIRIS Software Github - The OSIRIS software is now hosted on github. Historical descriptions are listed below.
Observing Planning GUI - OSIRIS observers can generate and save planning scripts, data definition files (.ddf), for observing with the spectrograph and imager by using the Observing Planning GUI. This java package will be identical to what you will be using at the telescope and requires java 1.4 or higher. To use, download and unpack the package and refer to the README file.
Quicklook2 Package - OSIRIS spectrograph frames are 3D FITS files that require sophisticated image visualization tools. The OSIRIS team presents an IDL based software package called Quicklook to display and analyze your OSIRIS data cubes. Quicklook is the OSIRIS image analysis software used at Keck while observing, but we also encourage using Quicklook for post-observing analysis of 2-D and 3-D fits frames. To use, simply download the tar file and unpack the file somewhere in your IDL path. Edit the environment variable 'QL_FILEDIR' in the file 'run_ql2' to match the directory path where you just unpacked Quicklook2.tar file. Once this environment variable has the correct path, you are ready to start using Quicklook2. Type 'run_ql2' at your terminal prompt within the same directory, and this script should launch Quicklook2 program and place the IDL xterm in an icon. In Windows, type 'run_wql2' at the IDL prompt. This software package supports the UNIX, LINUX, Mac OS, and Windows operating systems and operates on IDL versions 5.4 or higher.
Observing Planning GUI - OSIRIS observers can generate and save planning scripts, data definition files (.ddf), for observing with the spectrograph and imager by using the Observing Planning GUI. This java package will be identical to what you will be using at the telescope and requires java 1.4 or higher. To use, download and unpack the package and refer to the README file.
Quicklook2 Package - OSIRIS spectrograph frames are 3D FITS files that require sophisticated image visualization tools. The OSIRIS team presents an IDL based software package called Quicklook to display and analyze your OSIRIS data cubes. Quicklook is the OSIRIS image analysis software used at Keck while observing, but we also encourage using Quicklook for post-observing analysis of 2-D and 3-D fits frames. To use, simply download the tar file and unpack the file somewhere in your IDL path. Edit the environment variable 'QL_FILEDIR' in the file 'run_ql2' to match the directory path where you just unpacked Quicklook2.tar file. Once this environment variable has the correct path, you are ready to start using Quicklook2. Type 'run_ql2' at your terminal prompt within the same directory, and this script should launch Quicklook2 program and place the IDL xterm in an icon. In Windows, type 'run_wql2' at the IDL prompt. This software package supports the UNIX, LINUX, Mac OS, and Windows operating systems and operates on IDL versions 5.4 or higher.
- You may download example reduced OSIRIS cubes (broadband and narrowband) of star HD106965 for interacting with Quicklook2 -
OSIRIS Cube Kbb 0.1' and OSIRIS Cube Jn3 0.1'
Data Reduction Pipeline - Due to the unique nature of OSIRIS data and of its calibration steps, the OSIRIS team has developed a comprehensive pipeline designed to fully reduce all of the calibration data and to reduce scientific data to the level where an astronomer can begin custom analysis. The OSIRIS pipeline is designed to fix artifacts on the raw 2D array, wavelength calibrate, and assemble all the spectra into a 3D cube (λ wavelength, x and y spatially). In addition, after the 3D cube is assembled the pipeline allows for mosaicking of multiple frames with integer lenslet steps. The OSIRIS team is continually optimizing the pipeline and analysis tools for all users. However, unlike space-based data reduction pipelines, the general user is responsible for generating their own custom analysis tools for their specific scientific project. The OSIRIS team and other users have been developing stand alone analysis tools. We highly recommend and support a cohesive community for OSIRIS data reductions and analysis. Please see the OSIRIS manual for detailed instructions on how to install and run the data reduction pipeline.
Data Reduction GUI - The pipeline accepts commands only from XML (eXtensible Markup Language) files that we refer to as data reduction files (DRFs). Users may either hand edit these DRFs or use the java ODRFGUI package which generates DRFs with the user specifications. This GUI allows users to easily select pipeline modules, input directories, output directories, and execute scripts into the pipeline. This GUI should onlybe used with the version 2.0 or higher of the pipeline, and requires java 1.4 or higher. To use, download and unpack the package and consult the README file.
OSIRIS Updates - This website lists all the major hardware and software changes, and information on the calibration scans for OSIRIS. The pipeline uses a calibration scan for each independent mode (combination of filter and scale) to determine the spectral extraction and wavelength solution. Please use this page to determine which calibration scans you should be using for your observations.
OSIRIS Team
Osiris Macdonald
The OSIRIS team would prefer the following reference to be citedwhen referring to the instrument in publication:
'OSIRIS: a diffraction limited integral field spectrograph for Keck'
Larkin et al. 2006, Proceedings of the SPIE, Volume 6269, pp. 62691A (2006)
'OSIRIS: a diffraction limited integral field spectrograph for Keck'
Larkin et al. 2006, Proceedings of the SPIE, Volume 6269, pp. 62691A (2006)
OSIRIS Engineering Team: James Larkin, Matthew Barczys,Alfred Krabbe, Sean Adkins, Ted Aliado, Paola Amico, George Brims,Randy Campbell, John Canfield, Thomas Gasaway, Allan Honey, ChristofIserlohe, Chris Johnson, Evan Kress, David Lafreniere, Ken Magnone,Nick Magnone, Michael McElwain, Juleen Moon, Andreas Quirrenbach,Gunnar Skulason, Inseok Song, Michael Spencer, Jason Weiss, andShelley Wright
OSIRIS Commissioning Team: James Larkin, Matthew Barczys, Alfred Krabbe, Christof Iserlohe, Michael McElwain, Andreas Quierrenbach, Jason Weiss, and Shelley Wright
OSIRIS Keck Support Team: Jim Lyke, Randy Campbell, and Al Conrad
OSIRIS Data Reduction Pipeline Team: James Larkin, Shelley Wright, Jason Weiss, Mike McElwain, Marshall Perrin, Christof Iserlohe, Alfred Krabbe, Tom Gasaway, and Tommer Wizanski
OSIRIS Quicklook2 Package: Michael McElwain, Jason Weiss, Marshall Perrin, and James Larkin
OSIRIS Science Publications
(25 papers and running..)
'Diffraction-limited Imaging Spectroscopy of the Sagittarius A* Region Using OSIRIS, a New Keck Instrument'
Krabbe et al. 2006, ApJL, Volume 642, Issue 2, pp. L145-L148
Krabbe et al. 2006, ApJL, Volume 642, Issue 2, pp. L145-L148
'First High-Contrast Science with an Integral Field Spectrograph: The Substellar Companion to GQ Lupi'
McElwain et al. 2007, ApJ, Volume 656, Issue 1, pp. 505-514
McElwain et al. 2007, ApJ, Volume 656, Issue 1, pp. 505-514
'Integral Field Spectroscopy of a Candidate Disk Galaxy at z ~ 1.5 Using Laser Guide Star Adaptive Optics'
Wright et al. 2007, ApJ, Volume 658, Issue 1, pp. 78-84
Wright et al. 2007, ApJ, Volume 658, Issue 1, pp. 78-84
'Laser Guide Star Adaptive Optics Integral Field Spectroscopy of a Tightly Collimated Bipolar Jet from the Herbig Ae Star LkHα 233'
Perrin & Graham 2007, ApJ, 670, 499
Perrin & Graham 2007, ApJ, 670, 499
'Tvashtar awakening detected in April 2006 with OSIRIS at the W.M. Keck Observatory'
Laver, de Pater, & Marchis 2007, Icarus, 191, 749
Laver, de Pater, & Marchis 2007, Icarus, 191, 749
'Widespread Morning Drizzle on Titan'
Ádámkovics et al. 2007, Science, 318, 5852, 962
Ádámkovics et al. 2007, Science, 318, 5852, 962
'Integral Field Spectroscopy of High-Redshift Star Forming Galaxies with Laser Guided Adaptive Optics: Evidence for Dispersion-Dominated Kinematics'
Law et al. 2007, ApJ, 669, 929
Law et al. 2007, ApJ, 669, 929
'High-contrast imaging with Keck adaptive optics and OSIRIS'
McElwain et al. 2008, SPIE, 7015
McElwain et al. 2008, SPIE, 7015
'A Near-Infrared Variability Study of the Galactic Black Hole: A Red Noise Source with NO Detected Periodicity'
Do et al. 2009, ApJ, 691, 1021
Do et al. 2009, ApJ, 691, 1021
'The Role of Molecular Gas in Obscuring Seyfert Active Galactic Nuclei'
Hicks et al. 2009, ApJ, 696, 448
Hicks et al. 2009, ApJ, 696, 448
'The Kiloparsec-Scale Kinematics of High-Redshift Star-Forming Galaxies'
Law et al. 2009, ApJ, 697, 2057
Law et al. 2009, ApJ, 697, 2057
'Dynamics of Galactic Disks and Mergers at z~1.6: Spatially Resolved Spectroscopy with Keck Laser Guide Star Adaptive Optics'
Wright et al. 2009, ApJ, 699, 421
Wright et al. 2009, ApJ, 699, 421
'An OSIRIS Study of the Gas Kinematics in a Sample of UV-Selected Galaxies: Evidence of 'Hot and Bothered' Starbursts in the Local Universe'
Basu-Zych et al. 2009, ApJL, 699, L118
Basu-Zych et al. 2009, ApJL, 699, L118
'The global distribution of sulfur dioxide ice on Io, observed with OSIRIS on the W.M. Keck telescope'
Laver & de Pater 2009, Icarus, 201, 72
Laver & de Pater 2009, Icarus, 201, 72
'Component-resolved Near-infrared Spectra of the (22) Kalliope System'
Laver et al. 2009, Icarus, 204, 574
Laver et al. 2009, Icarus, 204, 574
'Probing young massive clusters with laser guide star adaptive optics'
McCrady, N. 2009, ApSS, 324,109
McCrady, N. 2009, ApSS, 324,109
'Evidence for strong dynamical evolution in disc galaxies through the last 11 Gyr. GHASP VIII - a local reference sample of rotating disc galaxies for high-redshift studies'
Epinat et al. 2010, MNRAS, 401, 2113
Epinat et al. 2010, MNRAS, 401, 2113
'The Presence of Weak Active Galactic Nuclei in High Redshift Star Forming Galaxies'
Wright et al. 2010, ApJ, 711, 1291
Wright et al. 2010, ApJ, 711, 1291
Osiris Macias Consultores
'Resolved spectroscopy of gravitationally lensed galaxies: recovering coherent velocity fields in subluminous z ~ 2-3 galaxies'
Jones et al. 2010, MNRAS, 369
Jones et al. 2010, MNRAS, 369
'Discovery of a Young L Dwarf Binary, SDSS J224953.47+004404.6AB'
Allers et al. 2010, ApJ, 715, 561 (using OSIRIS Imager)
Allers et al. 2010, ApJ, 715, 561 (using OSIRIS Imager)
'The Lick AGN Monitoring Project: The MBH - sigma Relation For Reverberation-Mapped Active Galaxies'
Woo et al. 2010, ApJ, 716, 269
Woo et al. 2010, ApJ, 716, 269
'The 2008 Outburst in the Young Stellar System Z CMa: The First Detection of Twin Jets'
Whelan et al. 2010, ApJ, 720L, 119W
Whelan et al. 2010, ApJ, 720L, 119W
'Near-infrared Spectroscopy of the Extrasolar Planet HR 8799 b'
Bowler et al. 2010, ApJ, 723, 850
Bowler et al. 2010, ApJ, 723, 850
'The Black Hole Mass in Brightest Cluster Galaxy NGC 6086'
McConnell et al. 2010, arxiv:1009.0750 U
McConnell et al. 2010, arxiv:1009.0750 U
'Measurement of a Metallicity Gradient in a z=2 Galaxy: Implications for Inside-Out Assembly Histories'
Jones, Ellis, Jullo, & Richard 2010, arxiv:1010.1538
Jones, Ellis, Jullo, & Richard 2010, arxiv:1010.1538
'Clouds and Chemistry in the Atmosphere of Extrasolar Planet HR8799b'
Barman, Macintosh, Konopacky, Marois 2011, arxiv:1103.3895
Barman, Macintosh, Konopacky, Marois 2011, arxiv:1103.3895
'The Nature of Double-peaked [O III] Active Galactic Nuclei'
Fu, Hai; Yan, Lin; Myers, Adam D.; Stockton, Alan; Djorgovski, S. G.; Aldering, G.; Rich, Jeffrey A, ApJ, 745, 67F
Fu, Hai; Yan, Lin; Myers, Adam D.; Stockton, Alan; Djorgovski, S. G.; Aldering, G.; Rich, Jeffrey A, ApJ, 745, 67F