Chandra Electronic Bulletin No. 20 |
******************************************************************************** | | | CCC XX XX OOO | Chandra | CC XX XX OO OO | CXC Electronic | CC XXX OO OO | Number 20 Bulletin | CC XX XX OO OO | December | CCC XX XX OOO | 2002 | | ******************************************************************************** Welcome to the Chandra X-ray Center's Electronic News Bulletin Number 20. CXC Web site: cxc.harvard.edu If you would like to unsubscribe from this alias, simply reply to this message to let us know. Please use this website to update your address or email: http://cxc.harvard.edu/cdo/udb/userdat.html Contents: 1. Astro-Statistics Workshop 2. Call for Proposals 3. WebGUIDE 4. ATOMDB V1.3.0 5. Announcing AstroAtom Website 6. ChaRT (Chandra Ray Tracer) ------------------------------------------------------------------------------- Item 1. Astro-Statistics Workshop ================================= Dear colleagues, We invite you to participate in a Post-AAS astro-statistics workshop: "Current Challenges in Poisson Multi-Scale Deconvolution Methods" January 15-16, 2003 Cambridge, Massachusetts (http://www.people.fas.harvard.edu/~vandyk/MultScaleConf/) This Post-AAS "Collaboratory" arises from Special Session 63: "Principled ``Model Free Deconvolution" via Multiscale Methods" (http://www.aas.org/publications/baas/v34n4/aas201/S630.htm) It was sparked by an unusual confluence: our key AAS speakers, their collaborators, and Boston-area multiscale and "deconvolution" experts from several disciplines will all be in the Boston area following the AAS. We are taking this opportunity to have: * two days of in-depth talks by key speakers; * commentaries by visiting experts; and * discussions by all. Participants are expected to range from students to seasoned reasearchers. GOALS: * Present the cutting edge of Poisson "deconvolution" techniques using new multiscale methods; * Hammer out current understandings, problems, and future challenges for Poisson multiscale methods across astronomy, medicine, engineering, and statistics; * Draft a list of questions, practical problems, challenges and new successes from the Special Session; * Provide a "gateway" for researchers new to these methods; and * Lay groundwork for new collaborations and new lines of research. * All with the goal of reporting back to the wider astronomical community. SPONSORED BY: * The Astronomy and Statistics Working Group at Harvard University, * The Statistics Group at Boston University, * NASA's AISR Program * The Chandra X-ray Center SCIENTIFIC ORGANIZING COMMITTEE: Alanna Connors, Eureka Scientific Peter Freeman, CXC/CfA Margarita Karovska, CXC/CfA Vinay Kashyap, CXC/CfA Eric Kolaczyk, Boston University Aneta Siemiginowska, CXC/CfA David van Dyk, Harvard University ------------------------------------------------------------------------------- Item 2. Chandra Cycle 5 Call for Proposals ========================================== On behalf of the Chandra Project and NASA, the Chandra X-ray Center is pleased to announce the release of the Cycle 5 Call for Proposals (CfP). The CfP invites scientists to participate in the Chandra X-ray Observatory's science program through proposing for new observations, for archival research projects or for theory/modeling projects in support of understanding Chandra data. The deadline for proposals is 7pm EST, 14 March 2003. The CfP may be found on the CXC web page at: http://cxc.harvard.edu/proposer/ We would like to draw your attention to the following items which are different from Cycle 4. Please refer to the Call for Proposals (CfP) and/or the Proposer's Observatory Guide (POG) for more information. ** Call for Proposals (CfP): For Cycle 5, the solicitation and selection of proposals has been delegated to SAO by NASA. As a result, this opportunity is announced by means of this CfP, rather than by a NASA Research Announcement (NRA) as in prior Cycles. ** Proposal Documentation: This has been reorganized. The Proposers' Observatory Guide (POG) includes instrument and satellite descriptions, while software and proposal preparation instructions have been replaced by web-based science threads. Please see the Proposers' Web page on the CXC website. ** Updated ACIS Effective Area: The ACIS effective area (AE) for Cycle 5 has been updated to account for the time-dependent decrease in the Quantum Efficiency of the ACIS chips. The AE provided is estimated to be that appropriate for the middle of Cycle 5, about May 2004. ** ACIS Bright Source X-ray Photon Dose Limitations: The CXC has adopted mission limits for the total photon dose per pixel in ACIS of: 2,500,000 cts/pix (FI) and 62,500,000 cts/pix (BI). If your observation calls for observing a bright point-like source close to on-axis, we suggest you use the MARX simulator (with the parameter DetIdeal=yes and dither, typically, on) to calculate whether your observation may reach 5% of the above mission limits in any one pixel. ** HRC Observing Modes: We have included a wider range of possible observing modes for the HRC detectors. It is now possible to select any combination of the detector (HRC-I/HRC-S), timing or regular mode and blocking filter. ** The observation visualizer tool (ObsVis): ObsVis has a few new capabilities including display of the satellite pitch angle (i.e., angle from the sun to the pointing direction) in addition to target visibility and satellite roll angle for a given sky position and the ability to display the default or selected ACIS chips in the Field-of-View figures. ** Observational Constraints: New possibilities for specifying observational constraints include: multiple (up to 4) window and roll constraints, geometric progression of observing windows for monitoring observations, and grouping a set of observations within a specified time period. ** TOO Response Time Bins: The classification of TOOs in terms of their response time has been updated to more accurately reflect the level of difficulty of responding to a request. ** Very Large Observing Projects: Up to 3 Msec of observing time will be available in Cycle 5 for projects requiring 1 Msec of observing time or more. Proposals of this type are encouraged and will be evaluated as described for Large Projects. There will be no proprietary time associated with Very Large Projects. ** New Joint Observing Programs: In Chandra Cycle 5 we will offer two additional joint programs, with the National Radio Astronomy Observatory (NRAO) and the Rossi X-ray Timing Explorer (RXTE). Similar to the joint program with NOAO, the Chandra peer review will be able to allocate time on NRAO telescopes and/or RXTE to sufficiently highly ranked proposals that require data from these facilities in addition to Chandra in order to address the scientific objectives. ** Listing of previous Chandra programs: Each proposal must include a list of all previous Chandra programs in which both the PI and the Observing Investigator (CoI identified as the primary contact) for the Chandra observations (if any) are/have been involved, including any papers resulting from those programs. ** Education and Public Outreach (E/PO): Management of the E/PO portion of the Chandra science program, including proposal receipt and review, and management of approved programs, has been transferred to the CXC for Cycle 5. ------------------------------------------------------------------------------- Item 3. WebGUIDE ================ We are pleased to announce WebGUIDE (http://obsvis.harvard.edu/WebGUIDE), an interactive web site that allows access to the atomic data found in ATOMDB. WebGUIDE currently has three functions. "Identify" creates a linelist based on a user-selected wavelength range and minimum emissivity. "Strong" creates a linelist of strong lines at a user-selected temperature around a user-selected wavelength range and minimum emissivity. Finally, "Describe" (available either from the main page or from a linelist created by Identify or Strong) lists the atomic parameters and references (actively linked to the ADS) for the data in ATOMDB. ------------------------------------------------------------------------------ Item 4 ATOMDB V1.3.0 ==================== ATOMDB V1.3.0 has been released as of Friday Dec 13, 2002. A major improvement will be the inclusion of K shell dielectronic recombination rates for Fe XVIII through Fe XXIV, complementing the existing Fe XXV and Fe XXVI data. These new rates were kindly provided by Dr. Verne Jacobs, based on the results published in Jacobs et al. (1989, Phys Rev. A, 39, 2411). The wavelengths have been adjusted to match solar and tokamak observations. V1.3.0 also corrects an error in the Li-like Ni XXVI line emissivities above 1e8 K (Thanks to Eugene Churazov). We have also fixed an error in some of the APED transition probabilities for hydrogenic ions (Thanks to Yair Krongold-Herrera). Note that this last problem does not affect line emissivity calculations for low-density collisional plasmas. See http://cxc.harvard.edu/atomdb for more information about downloading ATOMDB V1.3.0 and how to use it in fitting engines such as Sherpa, XSPEC, or ISIS. ------------------------------------------------------------------------------ Item 5. Announcing AstroAtom Website ======================================== Announcing AstroAtom: http://cfa-www.harvard.edu/astroatom/ We have completed work on a new website, AstroAtom, whose goal is to foster communication between astrophysicists and atomic physicists on areas of joint interest. This was a joint project of the CXC and Institute for Theoretical Atomic and Molecular Physics, so we are particularly interested in issues relating to high-energy astrophysics and atomic physics. The rationale for the website is that astrophysicists and atomic physicists have realized for some time that they need each other, and both communities have been attempting to increase communication between fields. However, cross-disciplinary work is difficult because we read different journals, attend different conferences, and largely work on different problems. The web is a natural vehicle to help to overcome some of these problems. For example, we imagine: * An astrophysicist using Chandra LETG data discovers a line around 70\AA, which could be either from Si IX or Fe XI. They post potential identifications to the website and asks if anyone knows of better wavelength measurements for these ions. * A laboratory atomic physicist replies that their group has data on Si IX wavelengths, and that a follow-up measurement could be done quickly if needed. * A theoretical atomic physicist replies that they have recalculated the Fe XI wavelengths and transition rates using a more accurate configuration interaction wavefunction and a paper is in progress. * Physicist replies that lab measurement of Fe XI wavelengths was done in 1992, published in the Canadian Journal of Physics. * And the entire thread is archived on AstroAtom for future reference. The website accepts postings (which are moderated to eliminate spam and other off-topic messages) from registered users, and also allows registered users to comment on posted material. Registration is free, and is only required to post messages or comments. All material on the site can be viewed and/or searched without registering. ------------------------------------------------------------------------------ Item 6. ChaRT (Chandra Ray Tracer) ================================== We are pleased to announce a release of ChaRT (Chandra Ray Tracer): http://cxc.harvard.edu/chart ChaRT is a user friendly web interface that allows the user to simulate High Resolution Mirror Assembly (HRMA) Point Spread Functions (PSFs) at any off-axis angle and for any energy or spectrum. ChaRT runs remotely the same code used internally at the CXC for PSF calibration, and it provides the user access to the best available mirror model, including many of the details of the HRMA's physical construction and a detailed model of the reflective properties of the mirror surface. ChaRT verifies and submits user's simulation parameters and notifies the user when their files are available for download via FTP. The output of ChaRT is a FITS table containing a collection of rays. In order to create a model PSF image it is necessary to project the rays onto the detector and take account of detector effects. This is achieved using the ChaRT rays as an input to MARX. A set of ChaRT threads accessible from the ChaRT web page were designed to guide the user: http://cxc.harvard.edu/chart/threads ------------------------------------------------------------------------------ This Electronic Bulletin is used for the dissemination of important announcements and information about the Chandra X-Ray Observatory to members of the community. If you wish to unsubscribe from the list, simply reply to this email to let us know. |
Last modified: 12/03/10
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