FUSE Cycle 8 Phase 1 Proposal Instructions Version 8.05, August 31, 2006 B-G Andersson 1. Introduction 2. FUSE Phase 1 Overview 2.1 Instrument Safety Concerns 2.2 Survey and Supplementary Programs 2.3 Special Requirements 2.4 Default Aperture and Aperture Selection 2.5 Target Acquisitions and Offset Targets 2.6 Signal-to-Noise Ratios in Individual Channels 2.7 Observations of Faint targets, NIGHT observations 2.8 Coordinated Observations 3. FUSE Phase 1 Proposal Keyword Definitions 4. Example FUSE Phase 1 Template Form Appendix A. FUSE Target Naming Conventions Web Links and Reference Material The FUSE Guest Investigator Web page is http://fusegi.pha.jhu.edu where the following are available: NASA Research Announcement, FUSE Cycle 8 GuestInvestigator Program. Guest Investigator Program Description and Proposal Instructions - Cycle 8. Phase 1 LaTeX Template File and Style File. The FUSE Science Center web page, http://fuse.pha.jhu.edu contains links to important reference documents and on-line tools. The FUSE Observer's Guide, version 8.0 http://fuse.pha.jhu.edu/support/guide/obsguide.html provides an overview of the satellite and includes descriptions of the telescope properties. It contains current reference information such as brightness limits and effective area curves. The FUSE Data Handbook, version 1.1 http://fuse.pha.jhu.edu/analysis/dhbook.html provides an overview of FUSE performance, data characteristics and procedures for data reduction and analysis. The FUSE Exposure Time Calculator (ETC) http://fuse.pha.jhu.edu/support/tools/exposure_time_tool.html is the most accurate way of estimating expected count rates andS/N ratios. The FUSE Blackbody UV Flux Calculator http://fuse.pha.jhu.edu/support/tools/bb_flux.html can be used to estimate expected continuum source fluxes in the FUSE wavelength range. Main Updates and Changes for Cycle 8 For Cycle 8, proposals are to be submitted fully in electronic form, mainly through the NSPIRES system at NASA Peer Review Services. This introduces important differences in the procedures for submitting the proposal from previous FUSE proposal cycles. All proposers must now fill in the Cover Page information and attach the formatted proposal at the NSPIRES web-site. The filled in LaTeX template form must still be submitted to fuseprop@pha.jhu.edu For non-US proposers, whose institutions are note registered in the NSPIRES database, NASA has created a special proposal organization, the "FUSE GI Support Center" to be the formal submitting organization. The Cover Page and formatted proposal cannot be submitted by the program PI, but must be submitted by an Authorizing Official ("Grants Administrator") at the PI institution. Under the new attitude control software, the sky availability of FUSE is more restricted than in cycles 1-6. However, the FUSE Project expects to be able to carry out some observations at low declinations during Cycle 8. Hence; Cycle 8 targets must be at absolute Declination greater than 50 degrees, except for certain low-declination targets as detailed in the "Proposal Instructions" and below. The FUSE bright limit is now 1x10^-10 erg cm^-2 s^-1 A^-1. For SiC only observation and for observations using LiF2 HIRS this limit is raised to 5x10^-10 erg cm^-2 s^-1 A^-1. The default aperture for HIST observations is again LWRS. Note, however, that the accumulated gain-sag causes a blurring of the spectra in HIST mode in certain parts of the detector. Hence for HIST observations requiring the highest possible spectral resolution, MDRS may be preferable (see further the FUSE Observer's Guide, section 2.5.3) A new keyword, \targtype{}, has been introduced to allow flagging of targets both for scientific priority and for low declination. The "NASA number" to be noted in the LaTeX template is the full string returned from the NPRS/NSPIRES site, not just its last three digits. The default "Guide camera" is Fine Error Sensor B (FES-B). As FES-B is associated with the Focal Plane Assembly for LiF2, the most reliable (and well centered) data will now occur in LiF2(A & B), rather than LiF1. The LaTeX style file is now fuse8.sty. 1. Introduction Guest Investigators (GIs) interested in obtaining FUSE data during Cycle 8 must complete and submit the Phase 1 proposal form. The main contents of a Phase 1 proposal are the scientific justification for the observations as well as their feasibility. These proposals will be peer reviewed by a committee of scientists. Based on the recommendations of the committee, NASA will select a certain number of programs for implementation. GIs whose programs have been selected will be required to submit a Phase 2 form where more detailed information will be required. Prior to submitting a Phase 1 form, GIs are requested to fill out a Notice of Intent to propose (NOI), accessible at the NASA Research and Education Support Services (NRESS) web site (http://nspires.nasaprs.com ). The deadline for submitting the NOI is August 4, 2006. Submittal of the NOI is not mandatory, but encouraged. A complete phase 1 proposal encompasses the Cover Page and attached formatted (in .pdf) proposal, submitted via the NSPIRES web site and the filled in LaTeX template form submitted to the JHU FUSE Science Center via fuseprop@pha.jhu.edu. Upon submital of the Cover page, the proposal will be assigned an identifier which constitutes a required keyword, \nasapropno{}, in the Phase 1 proposal. More information about using the NSPIRES system for FUSE Cycle 8 proposals is available on the FUSE GI web site (http://fusegi.pha.jhu.edu). This document contains the information necessary to complete a Phase 1 file for FUSE Cycle 8. Section 2 starts with an overview of the Phase 1 proposal process and goes on to describe general issues that proposers need to be aware of. Section 3 contains a description of the Phase 1 form, with detailed instructions on how to fill in each field. Section 4 contains a completed form for reference. The submission process for Phase 1 proposals is described in the NRA. Cycle 8 targets must be at absolute declinationd greater than 50 degrees, except for certain lower declination targets (see sections 1.3 and 2.1.3 of the "FUSE GI Program Description and Proposal Instructions"). The amount of observing time available at a given coordinate can be estimated from the sky maps of available observing time posted at the fusegi web site. Targets below absolute declination 55deg are generally considered to have marginal visibility. For targets below absolute declination 55deg or for those observations requiring more than 25% of the total visibility at that location, the Feasibility section of the proposal must include an assessment of the target wisibility (see the "Proposal Instructions" and the FUSEGI web site for further detail. The sky availability for Cycle 8 is limited to absolute declinations above 50 degrees. The FUSE project, however, expects to be able to expand the sky availability beyond this range during Cycle 8. A small number of observation of high scientific merit are expected to be possible at lower declinations. 2. FUSE Phase 1 Overview For Cycle 8 the FUSE proposal submission in fully electronic, but must be submitted, in parts, to two separate addresses. Hardcopy submittals are no longer required, nor accepted. The Phase 1 template file is an ASCII LaTeX file containing a set of keywords. Entries for some keywords are required, while entries for others are optional. Electronic submission of the completed LaTeX template file (without figures) is required of all proposers -- this file will be parsed and a database populated in order to support technical evaluation of the proposal. The proposers must also submit the formatted proposal together with the required Cover Page information through the NSPIRES system at NRESS. The formatted proposal can be conveniently generated using LaTeX along with the style file fuse8.sty provided by the FUSE project. (Instructions for retrieval of Phase 1 related material are given in the NRA.) The user canchoose to edit the Phase 1 forms using any text editor or useother software to generate the formatted proposal provided theformat given in section 2 of the NRA is followed. The Phase 1 form starts with several "front page" fields requesting contact information and summary details about the proposal. This is followed by text blocks for scientific justification, feasibility and safety analysis, and additional information. Next target and observation specific information is requested. The information is necessary for the planning personnel to perform a technical review of the proposal. The review includes an assessment of feasibility of the proposed observations and also addresses issues regarding instrument safety. GIs can use the on-line tools provided by the FUSE project to estimate count rates and expected signal to noise ratios. The use of these tools is strongly encouraged. Any situations not handled gracefully by the keywords can be further described in text blocks that are part of the Phase 1 submission. Very little instrument-specific information is requested from the proposer in Phase 1. 2.1 Instrument Safety Concerns The Phase 1 submission will include flux estimates for each target, as well as the signal to noise desired for each observation. The information provided will be used to determine whether the proposed observations are consistent with the capabilities of the instrument. FUSE has brightness and exposure limits for both continuum and emission line sources (see the FUSE Observer's Guide). Source fluxes extrapolated from longer wavelengths or based on models can be significantly in error, especially since the interstellar extinction at FUV wavelengths is often uncertain. The FUSE operations team will be cautious when dealing with any objects that are within a factor of 10 of the brightness limit and may require that a safety snap be performed (see next section on Special Requirements). The flux provided in the Phase 1 form would in general be at a reference wavelength that is of importance to the science. However, it may not be representative of the source brightness at other wavelengths in the FUSE bandpass. Therefore, it is extremely important that the peak fluxes expected from the proposed targets, and the uncertainties in the flux estimates be discussed in detail in the "Feasibility and Safety" text section. Emission line objects are a special case, since they seldom cause TOTAL flux or count rate problems but can still be a safety hazard for the FUSE detectors. The FUSE brightness limit applies at each wavelength - and a strong emission line from a source may violate that limit. It is requested that properties of the brightest emission line expected be used to populate the flux-related keywords (e.g.~surface brightness, line width). This should be done even if the brightest line is not the one of specific interest in the proposed scientific program. This is especially true for targets that are within a factor of 10 of the brightness limit. FUSE planners will assess the safety concerns based on the information provided. Therefore, methods of estimating the line flux and any uncertainties should be carefully described in the text. For example, if the line widths of the source are not well known and could introduce a brightness violation it should be stated explicitly in the proposal. 2.2 Survey and Supplementary Programs The program category "Survey and Supplementary" was introduced in Cycle 4 and continues to be offered in Cycle 8. This category allows GIs to submit proposals with scientific emphases somewhat different from that in "Standard" proposals. At the same time, these proposals help in maintaining scheduling flexibility without loss of observing efficiency. "Survey and Supplementary" programs are for projects involving the survey of a class of objects or alternatively for providing supplementary data of scientific importance on some set of targets. In either case, the GI lists a number of proposed targets (there is no restriction on the number, and may be as low as one) and if the proposal is accepted, these targets are put into the database of objects to be scheduled for observation. However, the scheduling priority is lower for these objects than for "Standard" targets and any given object will be observed only if it is advantageous to the scheduling plan.The decision whether to observe a target or not is driven solely by the requirements of FUSE mission planning. "Survey and Supplementary" targets must also be constrained to absolute Declination above 50 degrees. "Survey and Supplementary" programs have some advantages. If a prospective GI is interested in a class of objects (say, Algol binaries) and would like to obtain FUV spectra of as many as possible, that person could propose a list of targets. If the proposal is accepted, some fraction of the objects on the list will be observed. The scientific justification for such a proposal would not be focused on one or a few objects but rather on why FUSE observations of Algol binaries are important. The object class need not be the link among the targets proposed. The link may be, for instance, the properties of the sight-lines proposed. Although it is expected that data will be obtained for most accepted "Survey and Supplementary" programs, the drawback is that a specific object may not be observed. Also, there is no minimum executed observation time guaranteed for an accepted survey program. 2.3 Special Requirements Special Requirements (SRs) flag the system to some supported modes of observation that are relatively infrequent, or to situations which require special attention on the part of the planners. There is a text block in the Phase 1 form fordescribing the proposed observations. Justification for any desiredSRs must be included in this section. The SRs also need to be entered,where needed, at the appropriate places in the target lists. If more than one SR applies, all should be supplied with individual entries separated by commas. Observations with SRs often constrain the scheduling and are sometimes lower observation efficiency (since they require special handling) so SRs should be requested only when the need is there. For cycle 8, most of the earlier available SRs will not be allowed. Special Requirements supported in Cycle 8: TOO: "Targets of Opportunity" come in two varieties -- those with unknown position, and those with known position but unknown observation timing constraints. The TOO SR flags the Phase 1 parser that much of the information normally required (such as co-ordinates and fluxes) may not be present in the Phase 1 form. The likelihood that the TOO might occur during the observing cycle should be discussed in the "Description of Observations" text section. FPSPLIT: Very high signal-to-noise ratios (>30) can be achieved using a focal plane split observing procedure, which may be requested via this SR. The total integration time requested will be split into 4 nearly equal parts with the FPAs and mirrors moved by a small amount between observations. It is important to note that to achieve a given S/N, the total time required is larger (by a factor of 2-4) than that simply determined by photon statistics. This point has been explicitly discussed in theFUSE Observer's Guide, v8.0, and in a FUSE white-paper linked at that web page which the GI are urged to consult. SNAP: Used to specify an observation for which a preliminary, relatively short observation is requested. The shorter observation is typically needed to verify the flux or demonstrate feasibility prior to a longer observation. Operationally, the GI will inspect the SNAP spectrum and notify the FUSE project that the main observation may be scheduled. In the Phase 1 target listing, SNAP targets should be listed twice: once with the SNAP SR and the exposure time for the SNAP, and once for thescience observation without the SNAP SR. It may be that a pool of SNAP targets is proposed with a follow-up observation of the best candidate. Such issues should be discussed in the text. SAFTSNP: For targets where the fluxes are near the brightness limits, and/or the FUV flux is very uncertain, a "safety snap" is required, and the SAFTSNP SR should be used. Large overheads are involved when scheduling SAFTSNP observations and each such observation is charged 2000 seconds (even if the on-target exposure time is short). For the Phase 1 entry, \integrationtime a value of 2000 seconds should be entered for SAFTSNP observations. Actual times will be calculated by FUSE planners before implementing the observation. As with regular SNAPs, the SAFTSNP and science observation (with real estimated exposure time) should be entered as separate items. See the FUSE Observer's Guide for more information. 2.4 Default Aperture and Aperture Selection Due to intermittent problems with Fine Error Sensor A (FES-A), initially encountered in the spring of 2005, the FUSE project switched to FES-B as the default Guide Camera in July 2005. As FES-B views the Focal Plane Assembly (FPA) in the LiF2 channel, the most reliable (and well centered) data will now occur in LiF2(A & B), rather than in LiF1. After the FUV focus in LiF2 was optimized early in the mission, the image quality in FES-B was found to be marginal for guiding purposes. In order to improve the image quality in FES-B, the LiF2 FPA has been moved to a position that is offset from the focal plane of the LiF2 primary mirror. The spectral resolution in LiF2 is unaffected for observations of point sources, but the throughput of the narrow apertures will be reduced. The effective transmission of the apertures has not been characterized in detail, but is approximately 70% for MDRS and 15% for HIRS. These factors have been incorporated into the on-line Exposure Time Calculator (ETC). The resolution for observations of diffuse sources in LiF2 is expected to degrade slightly (see the FUSE Observer's Guide, v8.0 for details). During the science verification period soon after launch, it was seen that thermal effects caused channel alignment to vary on orbital time scales as well as during slews between targets. With careful planning the alignment can be maintained sufficiently well that point sources are within the LWRS aperture in all 4 channels. Furthermore, it was found that the spectral resolution achieved for point sources (especially if observed in time-tag mode) was about the same for LWRS and MDRS observations. This is particularly true for the LiF data. The spectral resolution in the SiC channels, and for histogram data is slightly lower for LWRS observations (see the FUSE Observer's Guide for more information). As a result of these findings, it was determined that the LWRS (30x30 arcsec) would be the default observing aperture. Data aquired in the fourth and fifth years of operation indicated that the cumulative effect of all observations performed since the beginning of the mission had at that time measurably depleted the available charge on the FUSE detectors at certain wavelengths at the location corresponding to the LWRS aperture. For HISTOGRAM mode observations where pulse-height information is not available for each detected photon, this can lead to significant deterioration of the derived spectrum. In order to preserve sensitivity for faint targets (which do not allow FUV PEAK-UPs), the default aperture for bright target (HIST) observations were, therefore, changed to the MDRS aperture in June 2004. However, due to the alignment difficulties associated with MDRS observations, the default aperture for all observations have been reset to LWRS for Cycle 8. Observations with the MDRS (4x20 arcsec) or HIRS (1.25x20 arcsec) apertures are preferable in certain situations. For instance to minimize the contamination from terrestrial airglow emission or for HIST observations where the wavelength regions most affected by the charge depletion are essential for the analysis. (see the FUSE Observer's Guide, v8.0 for details). If the wavelength range of interest islongward of about 1000 A, observations using the smaller apertures arepossible. This is because the LiF alignments are relatively well behaved.GIs may want to modify the requested integration time based on lower totaleffective area available. The LiF 2 channel is linked to the Fine Error Sensor that is used to guide and therefore always maintains alignment. For observations where the HIRS aperture is requested, only LiF 2 coverage is guaranteed. Full wavelength coverage using the MDRS apertures is possible forobjects with sufficient FUV flux to allow peak-up acquisitions(see next section). The procedure for observing may requiremultiple peak-ups per orbit for re-aligning the channels. This will have an impact on operational efficiency and may bedifficult to schedule. Hence GIs requesting MDRS aperture observationsmust specify whether SiC (i.e., short wavelength) coverage is essential, desirable, or not necessary for the science proposed. This will allow the operationalimpact of the request to be assessed properly. Note that requiring SiC data puts additional planning constraints on the observation. If these cannot be met at an otherwise opportune time, the observation will be delayed. The need for MDRS or HIRS apertures must be explicitly discussed in the Phase 1 proposal. The short wavelength requirement for MDRS observations must likewise be included. The discussion can be in either the scientific justification section or the feasibility section, at the GIs discretion. 2.5 Target Acquisitions and Offset Targets When observing with the LWRS apertures, acquistion proceduresare usually simple. Guide stars are selected around the targetposition. The coordinates are assumed to be accurate in theHST Guide Star reference frame, and the target is placed inthe LWRS apertures. (This procedure is called "guide star acquisition".) Guide star acquistion may be sufficient to place a target in theMDRS apertures, but even then the issue of channel alignment needsto be addressed. If the target is bright enough in the FUV,"peak-up acquistion" can be performed. The target is placed nearthe MDRS apertures which are then stepped along the X co-ordinate(i.e., across the aperture width). The onboard instrument computerprocesses the data and aligns the channels based on the positionwhere fluxes are maximized. This procedure works well for initialalignment but lasts only about 10 minutes, particularly for the SiC channels (note that LiF 2 will stay aligned). Therefore multiple peak-ups during an observation may be necessary. Peak-up acquisition can be used for the HIRS apertures as well, but the time scale for misalignment to occur is much shorter. Hence, only LiF 2 data is guaranteed for observations requesting HIRS. Extended targets (using any of the apertures), and MDRS observations of targets that are too faint in the FUV to acquire with peak-ups will need alternative acquistion procedures. These usually entail the use of an offset star or an offset field. Such observations are not very frequent, so we refer GIs to the FUSE Observer's Guide for details about offset star acquistion. Note that offset stars are not requested as separate targets in Phase 1. However, the need and availability of appropriate offset stars should be discussed in the "Description of Observations" text block. Offset stars will have to be specified explicitly in the Phase 2 submission. 2.6 Signal-to-Noise Ratios in Individual Channels Combining data fromthe different channels usually results in lowering the spectralresolution. Also, handling the statistical errors in such a data combination correctly iscomplicated. Therefore, in many cases GIs may want to consider thesignal to noise that will be obtained from an individual channel of thespectrograph. The on-line tools (e.g. the Exposure Time Calculator andthe Count Rate Tool) were updated prior to Cycle 3 to allow the calculation of signal-to-noise for individual channels as well as forthe sum of all channels. A new keyword was also introduced into thePhase 1 form that let the proposer specify the channel assumed for theS/N calculation. These updates will hold through Cycle 8. It isimportant that proposers describe their S/N calculations andassumptions in the feasibility text section. The use of the on-linetools is strongly encouraged. 2.7 Observations of Faint targets, NIGHT Observations Observations of faint (<3x10^-15 erg cm^-2 s^-1 A^-1)sources, particularly through the LWRS apertures may be compromised byterrestrial airglow emission. The airglow problem can be significantlyreduced by analyzing data taken only during the night-time portion ofthe observation. FUSE cannot be easily re-targeted within orbits, soscheduling "night-only" observations is extremely inefficient and isNOT supported. If an observation requires night-time data, then theproposer should request a total observation time that is long enough to obtain the desired night exposure. Experience has shown thatfor a typical observation, the total exposure time is about 1.6 timesthe night exposure time. If an observation requires 10,000 seconds ofexposure time at night, the proposer should request 1.6*10,000 = 16,000seconds for the observation. 2.8 Coordinated Observations For any number of scientific reasons coordinating FUSE observationswith other space-based or ground-based facilities may be desirable. Operational constraints, however, make coordinatedobservations very difficult and often extremely inefficient toschedule. Even modest coordination (at the several week level) canhave a significant effect on overall scheduling over some longer timeperiod. The FUSE project recognizes the scientific importance of co-ordinated observations and will support a very limited number of such requests on a best effort basis. Under the present attitude control scheme it is unlikely that a "simultaneity" better than several weeks can be achived. The needfor co-ordinated observations should be discussed in detail in the "Additional Information" text block in the Phase 1 form. While co-ordinated observations may be requested at thePhase 2 stage, acceptance for such requests will be contingent on the explicit approval of the FUSE project scientist. 3. FUSE Phase 1 Proposal Keyword Definitions In this section we step through the Phase 1 form and describe the keyword entries and the text block requirements. Note that comments in the template are preceded with a "%" sign (LaTeX syntax). Proposers can add comments to the form for their own convenience, but these will not be processed by the Phase 1 ingestion software nor will they be read by FUSE personnel. Keyword values are generally inserted between the curly brackets. In some cases a list of options is given in the form of comments. Then, one of the entries in the list must be un-commented by deleting the "%" sign. Text for the text blocks should be inserted below the appropriate keyword. An example form showing the syntax for keyword values is given in Section 4. Helpful guidelines are included in the Phase 1 template file. Please use the most recent template and style files -- these can be downloaded from the FUSE website. 1. Proposal Title \title{} % (Required) The program title should be as short and descriptive as possible and should be no longer than two lines in the formatted output. (This limits the title to about 100 characters.) 2. NASA Proposal Number \nasapropno{} % (Required) This keyword allows cross-referencing between NASA Peer Review Service proposal numbers and those used by the FUSE project. Enter the identifier assigned to the "Cover Page" submitted to NASA NSPIRES proposal processing web site. The identifier is of the form 06-FUSE8-123. 3. Principal Investigator Contact Information (All Fields Required) \pititle{} [e.g. Dr., Mr., Ms., Prof., etc. ] (All required) \pifirstname{} [e.g. John, or John G. to include middle initial] \pilastname{} \piaffiliation{} [e.g. Department of Astronomy, etc.] \institution{} [e.g. your university or institute name] \address{} [e.g. 123 East St., Baltimore, MD 21218] \country{} [e.g. USA, SWE, IND, etc.] \phone{} \fax{} \email{} [e.g. you@somewhere.anywhere.edu] All requested contact information should be supplied for the principal investigator (PI). The PI is the primary contact for questions about the program. Non-US proposers using the "FUSE GI Support Center" as their formal submittal organization should still list their nominal home institution here. 4. Scientific Category (Required) %\scientificcategory{COOL STARS AND PROTOPLANETARY SYSTEMS} %\scientificcategory{WHITE DWARFS AND CATACLYSMIC VARIABLES} %\scientificcategory{HOT STARS AND MASSIVE BINARIES} %\scientificcategory{STELLAR EJECTA AND GASEOUS NEBULAE} %\scientificcategory{INTERSTELLAR MEDIUM AND GALACTIC STRUCTURE} %\scientificcategory{GALAXIES AGN AND QUASARS} %\scientificcategory{INTERGALACTIC MATERIAL} Select a primary scientific category for your proposal by uncommenting the appropriate line from the list. 5. Observing Program Category (Required) %\programcategory{STANDARD} %\programcategory{SURVEY} Each Cycle 8 proposal must be identified as either a "Standard" or "Survey" proposal. Standard proposals correspond to regular observing programs and may contain constrained observations (see NRA Section 1.2, 1.3). Survey proposals provide the opportunity to observe a class of objects without the requirement that a specific target be observed. No constrained observations are allowed in Survey programs, and all targets must be at |dec|>50 degrees. THE SELECTED CATEGORY MUST APPLY TO ALL TARGETS IN THE PROPOSAL. Select a single category for your proposal from the choices given below by uncommenting the appropriate category. 6. Observation Summary Information \totalobstime{} % (Required, in ksec) \totalobjects{} % (Required) The \totalobstime keyword value should be the total requested observation time in kiloseconds for all targets in the program. To calculate this, any observations with \integrationtime less than 4000 seconds should be accounted as 4 kiloseconds. Any SAFTSNP exposures, which are likely to be very short should be accounted as 2000 seconds. This is done because of the relatively large overhead needed for observations with short exposure times. See the FUSE Observer's Guide for more information. The \totalobjects keyword value is the number of independent positions on the sky that are proposed. Different positions on extended sources should be counted as separate targets. 7. Abstract (Required, text block) \begin{abstract} \end{abstract} Enter a brief description of the proposal between the \begin{abstract} and \end{abstract} commands. The goals of the program should be summarized. The abstract should fit on the front page of the formatted proposal and is therefore restricted to 200 words. The abstracts for all successful proposals will be made available on-line. In this and other text blocks do not use colons (":"). This causes problems with the proposal ingestion software. (However, keyword values such as the RA and DEC require colons.) 8. Co-I Information (Required for all Co-investigators) \begin{investigators} % List each Co-Investigator (CoI) by replicating the following seven % items for each CoI. If you have no CoIs, leave these lines unchanged. \coititle{} \coifirstname{} \coilastname{} \institution{} \country{} \phone{} \email{} \end{investigators} The format is similar to the entries for the PI, but less information is requested. 9. Scientific Justification (Required, text block) % Enter text after the \justification keyword. % <=3 pages, including figures, tables and refs. \justification Describe the scientific justification for the proposed program, stating clearly its goals and significance to astronomy. Brief discussions of the scientific background and previous work done on the subject should be included. The scientific reasons why FUSE data are needed should be discussed. The Scientific Justification (including figures, table and references) is limited to three pages. Other text blocks are provided for further descriptive material about the program. 10. Feasibility and Safety (Required, text block) % Enter text after the \feasibility keyword. % <=2 page \feasibility A detailed description of the signal-to-noise and spectral resolution requirements for the proposed observations should be included. (It should be explicitly mentioned whether the estimates apply to data from individual channels or the total.) The method and quality of the target flux estimates must be described, particularly if there are any concerns for instrument safety (typically targets that are close to or may possibly violate the bright limit). Describe the method used to estimate exposure times. the use of the on-line exposure time calculator is strongly encouraged. Up to two pages can be used for this section. 11. Description of Observations (Optional, text block) % Enter text after the \describeobservations keyword. % <=1 page \describeobservations Additional information about observation strategy can be included in this optional text block. Examples include: discussion of any supported Special Requirements special scheduling issues indicating high proper motion targets and position corrections any KNOWN special acquisition issues, including crowded field, proximity to bright object in field, need for blind offset acquistion, etc. 12. Additional Information (Optional, text block) % Enter text after the \additionalinfo keyword. % <=1 page \additionalinfo Up to one page of text can be included here to describe anything about the proposed program that the review panel may find useful. This section is not for adding to the scientific justification. Examples of what may be included here are: Data analysis plans or data modeling capabilities. Need to coordinate observations with other facilities. (This requires strong scientific justification as well.) Anything else that cannot readily be communicated via the target keywords or other text blocks. Cross referencing between any common target names used in the text and official names listed in the target list (according to the guidelines inAppendix A). 13. Previous FUSE Observing Programs (Optional, text block) % Enter text after the \previousfuseprograms keyword. % <= 1 page \previousfuseprograms Summarize the status of any FUSE programs the PI has from earlier cycles. Previous programs that the Co-Is have may be included but would be less important. The section has a limit of one page (including figures). 14. Investigator Information (Optional) % <= 1 page \vita A short biographical sketch of the PI may be presented here. Publications relevant to the proposal may be included. Such information about CoIs may also be included here at the proposer's discretion, but the total length of this section must not exceed one page when formatted. 15. Target List and Observation Summary (Required) \begin{observations} Repeat keywords as necessary for each target to be observed. In the formatted proposal, this information will come out in tabular format on a separate page or pages at the end of the proposal. \objectname{} % (Required) Object naming conventions and syntax follow those developed for use in HST proposals. Please refer to Appendix A below for FUSE target naming conventions. If other names are used in the proposal text, provide cross references in the "Additional Information" text block. \ra{} % (Required) \dec{} % (Required) Coordinates in standard astronomical format (HH:MM:SS.SS and [+/-]DD:MM:SS.S), referenced to the J2000 equinox, are required. The most accurate coordinates available should be provided. Accuracy to at least 5 arcsec is required for target duplication checks. \vmag{} % (Required for continuum sources) Johnson V magnitude or equivalent. \spectype{} % (Required) Provide MK spectral type and luminosity class for all stellar objects. Multiple entries are allowed for unresolved binaries, but no spaces are permitted. Hence, O7Ve+WN6 is allowed, but B3 III is not. For other types of sources, choose the best abbreviation from the following list of object types: QSO, AGN, GAL (galaxy), CV (cataclysmic variable), PN (planetary nebula), SNR (supernova remnant), CSPN (central star of planetary nebula), PSR (pulsar), REF (reflection nebula), CLU (cluster of galaxies), or OTR (other). \colorexcess{} % (Optional) Measured E(B-V), if available. The next set of keywords define the flux and source type information necessary for checking telescope safety, feasibility and verifying the expected signal-to-noise. % Source type: (uncomment only one) (Required) %\sourcetype{PC} % Point Continuum %\sourcetype{PE} % Point Emission-line %\sourcetype{EC} % Extended Continuum %\sourcetype{EE} % Extended Emission-line A two-letter mnemonic is entered, indicating first whether the source is point-like (P) or extended (E), and secondly whether it is primarily a continuum (C) or emission-line (E) source. For FUSE, any source smaller than 2 arcsec is point-like. In cases with both continuum and emission lines, the user should choose the one more important to the scientific program. This flag affects the interpretation of some of the entries given below (for instance, the units of "flux") and should be consistent with the other data entered. FUSE mission planners need to know of any special situations that might be safety concerns. For instance, if the continuum level of a symbiotic star was of primary scientific importance then the source type would be "PC" and the subsequent entries would follow appropriate to this designation. However, the peak line intensities of expected emission lines should be discussed in the "Feasiblity" text block so it can be verified that fluxes are below the detector bright limits. \lambdaref{} % (Required) The reference wavelength in Angstroms (A) should be entered. This should be a wavelength within the FUSE range (i.e. 905 - 1187 A). The flux and S/N entered should pertain to this wavelength. As such it should be a wavelength that is of interest to the proposed scientific program. For emission line sources the wavelength of the strongest expected line from the source should be chosen. \fluxlambdaref{} % (Required) The user should enter the flux at the reference wavelength. The flux should be written as n.nnE-nn format (where each "n" is a single-digit integer - please, no TeX formatting commands!). The value should be the flux at the telescope. That is, it should be corrected for interstellar extinction. The units are ergs/(cm^2 s A) for continuum sources, and ergs/(cm^2 s)(integrated line flux) for emission linesources. For extended sources, the flux should be the total flux expected through the selected aperture. Refer to the FUSE Observer's Guide for important information on brightness limits for continuum and emission line sources. % Flux estimate accuracy: (uncomment one) (Required) %\fluxaccuracy{HIGH} % HIGH %\fluxaccuracy{MED} % MED %\fluxaccuracy{LOW} % LOW This keyword is used to indicate the accuracy level of the flux information provided above. It is important for both safety and onboard memory usage estimation. As a guideline, HIGH should indicate an actual observed valuein the FUSE range (say 1200 Å or below, from FUSE, IUE, HUT, ORFEUS, or HST)or a small extrapolation from <=1300 Å MED should indicate situationswhere extrapolation from longer UV wavelengths was required, or wheresome model-dependent or extinction uncertainty is involved; LOWindicates uncertain estimates either because the extrapolation is from much longer wavelengths, or the source flux is not well understood in the FUV, etc. % Info for emission line or extended objects. % Uncomment next 2 keywords if they apply: %\elinefwhm{} %(Required for \sourcetype = PE and EE) %\sblambdaref{} %(Required for \sourcetype = EC and EE) The \elinefwhm{} keyword entry is required only for emission line sources. Enter the FWHM of the line in decimal A. The \sblambdaref{} keyword entry is required only for extended sources. Enter the expected surface brightness at the reference wavelength in flux units per square arcsecond. The format is n.nnE-nn (no TeX formats allowed). \resolutionelement{} % (Required) This field is the resolution element, in A, for which the quoted signal-to-noise ratio has been calculated. The smallest meaningful resolution element value allowed is 0.05 A, whichis the measured instrumental resolution. Larger values can be entered, depending on the scientific goals of the proposal. The data will always be obtained at highest possible resolution and any binning will be left to the user. \signoisechan{} % (Required) The signal-to-noise can be calculated for individual channels or for the total of all channels available at a given wavelength. The entry to this keyword specifies the channel for which the S/N is listed. Valid entries: SIC1, SIC2, LIF1, LIF2, or TOTAL. \signoise{} % (Required) The expected signal-to-noise per resolution element at the reference wavelength for the channel (or TOTAL) specified should be entered here. The maximum S/N per default (0.05 Å) resolution element is 30. Higher S/N values can be obtained using the special FSPLIT procedure (see Section 2). % (Required) % LWRS (30"x30") (Default) \aperture{LWRS} % MDRS (4"x20") %\aperture{MDRS} % HIRS (1.25"x20") %\aperture{HIRS} LWRS is the default channel. Comment out LWRS and uncomment one of theother channels to change the aperture requested. Any request for MDRSor HIRS should be justified in the "Description of Observations" text block. % Special requirements: (uncomment all keywords that apply) % (Optional, as needed) %\specialreq{TOO} %\specialreq{FPSPLIT} %\specialreq{SNAP} %\specialreq{SAFTSNP} Special requirements that will be supported for Cycle 8 are TOO, FSPLIT, SNAP and SAFTSNP. These are describedin Section 2, above. Uncomment all SRs that are needed for a target. % Change by commenting out B and un-commenting other. (Only one must be % un-commented.) For STANDARD program-category proposals a mix of target % types A & B is allowed. For SURVEY program-category proposals only target- % type D is allowed. % % Target Type (Required) % %\targtype{A} \targtype{B} %\targtype{C} %\targtype{D} To allow a more direct identification of the scientifically most important targets for FUSE to observe in Cycle 8, the keyword \targtype{} has been added. This keyword is also used to identify low declination targets to be observed if and when this capabillity is again available. The four options are A: the scientifically most important targets, which will be allowed to drive the FUSE scheduling and may significantly impact the observing efficiency. Only a limited number and total exposure time will be allowed of this target type. B: Regular STANDARD program- category targets, C: targets below the nominally accessible Declination range (|dec|>50deg) and D: SURVEY program-category targets. \integrationtime{} % (Required) The on-source integration time requested for an observation should be entered here, in units of seconds. For SNAP observations, this is the length of the shorter test exposure; a separate target entry should be provided for the proposed science observation. For SAFTSNPs, enter 2000 seconds (for accounting purposes only). 4. Example FUSE Phase 1 Template Form The template included below has many of the comment lines deleted, and is meant only to give the proposer an idea about the layout of the form. The proposer should download and use the Phase 1 form available at the FUSE website. It contains detailed comments and additional instructions. % FUSE Phase 1 observing proposal LaTeX template (version 8.0) % For Cycle 8 % \documentclass[12pt]{article} \usepackage{fuse8} \begin{document} % 1. Proposal Title \title{Observations of a Twinkling Star} % (Required) % 2. NASA Proposal Number \nasapropno{06-FUSE8-234} % (Required) % 3. Principal Investigator Contact Information. (All Fields Required) \pititle{Mr.} \pifirstname{Johns} \pilastname{Hopkins} \piaffiliation{Board of Directors} \institution{Baltimore and Ohio Railroad} \address{111, Railway St., Baltimore, MD 21000} \country{USA} \phone{410-111-1111} \fax{410-222-2222} \email{jh@bando.rail.com} % 4. Scientific Category (Required) %\scientificcategory{COOL STARS AND PROTOPLANETARY SYSTEMS} %\scientificcategory{WHITE DWARFS AND CATACLYSMIC VARIABLES} \scientificcategory{HOT STARS AND MASSIVE BINARIES} %\scientificcategory{STELLAR EJECTA AND GASEOUS NEBULAE} %\scientificcategory{INTERSTELLAR MEDIUM AND GALACTIC STRUCTURE} %\scientificcategory{GALAXIES AGN AND QUASARS} %\scientificcategory{INTERGALACTIC MATERIAL} % 5. Observing Program Category (Required) \programcategory{STANDARD} %\programcategory{SURVEY} % 6. Observation Summary Information % Total observing time, in Kiloseconds \totalobstime{40} % (Required) % Total number of objects \totalobjects{1} % (Required) % 7. Abstract (Required, text block) \begin{abstract} Enter abstract text here. In this and other text blocks do not use colons (":"). This causes problems with the proposal ingestion software. (However, keyword values such as the RA and DEC require colons.) \end{abstract} % 8. Co-Investigator Information (Required for all Co-investigators) \begin{investigators} \coititle{Dr.} \coifirstname{Henry} \coilastname{Rowland} \institution{Johns Hopkins University} \country{USA} \phone{410-516-0000} \email{rowland@pha.jhu.edu} \end{investigators} % 9. Scientific Justification. (Required, text block) % <=3 pages, including figures, tables and refs. \justification Enter justification here. Figures may be included. %Include Figure \begin{figure}[h] \plotone{image.eps} \caption{image worth a thousand words} \end{figure} % 10. Feasibility and Safety. (Required, text block) % <=2 page \feasibility Enter text here. % 11. Description of Observations. (Optional, text block) % <=1 page \describeobservations Enter text here. % 12. Additional Information. (Optional, text block) % <=1 page \additionalinfo Enter text here. % 13. Previous FUSE Observing Programs. (Optional, text block) % <= 1 page \previousfuseprograms Enter text here. % 14. Investigator Information. (Optional, text block) % <= 1 page \vita Founded university. %---------------------------------------------------------------------- % 15. Target List and Observation Summary %---------------------------------------------------------------------- \begin{observations} % see Appendix A of Phase 1 instructions for conventions % NOTE THAT THERE MUST NOT BE ANY SPACES IN THE TARGET NAMES. \objectname{HD4515} % (Required) % Should be in the form HH:MM:SS.SS (J2000 equinox) \ra{45:45:45.45} % (Required) % Should be in the form DD:MM:SS.S (J2000 equinox) \dec{15:15:15.3} % (Required) % Visual magnitude, Johnson V magnitude preferred \vmag{12.1} % (Required) % Enter a spectral type. For stars, provide the MK spectral type % and luminosity class (no spaces! example: O7Ve). % For non-stars use one of the following: % QSO, AGN, GAL, SOL, CV, PN, SNR, CSPN, PSR, REF, CLU, OTR. % (CLU=cluster of galaxies; OTR=other) \spectype{B0V} % (Required) % Measured E(B-V) \colorexcess{0.03} % (Optional) % Source type: (uncomment only one) (Required) \sourcetype{PC} % Point Continuum %\sourcetype{PE} % Point Emission-line %\sourcetype{EC} % Extended Continuum %\sourcetype{EE} % Extended Emission-line % Reference wavelength in Angstroms \lambdaref{1030} % (Required) % Estimated, observed, flux value at wavelength \lambdaref. in erg/cm2/s/A % Example: \fluxlambdaref{1.5e-12} % NO TeX formatting allowed in this keyword. \fluxlambdaref{1.2e-12} % (Required) % Flux estimate accuracy: (uncomment one) (Required) %\fluxaccuracy{HIGH} % HIGH \fluxaccuracy{MED} % MED %\fluxaccuracy{LOW} % LOW % Info for emission line or extended objects. % Uncomment next 2 keywords if they apply: % FWHM of line in Angstroms for emission line objects %\elinefwhm{} %(Required for \sourcetype = PE and EE) % Surface brightness at wavelength \lambdaref in erg/cm^2/s/A/arcsec^2. % (Required for \sourcetype = EC and EE) % Example: \sblambdaref{1.2e-15} % NO TeX formatting allowed in this keyword. %\sblambdaref{} %(Required for \sourcetype = EC and EE) % Size of resolution element in Angstroms \resolutionelement{0.1} % (Required) % Channel used to calculate the S/N: SIC1, SIC2, LIF1, LIF2, or TOTAL \signoisechan{LIF2} % (Required) % Expected S/N per resolution element \signoise{20} % (Required) % Aperture: (LWRS is default, change by commenting out LWRS and % un-commenting other. Only one must be un-commented) % (Required) % LWRS (30"x30") (Default) %\aperture{LWRS} % MDRS (4"x20") \aperture{MDRS} % HIRS (1.25"x20") %\aperture{HIRS} % Special requirements: (uncomment all keywords that apply) % See phase 1 proposal instructions for details % (Optional, as needed) % Target of opportunity %\specialreq{TOO} % FPSPLIT observing procedure required (high S/N observation) %\specialreq{FPSPLIT} % Short exposure (snapshot) before follow up %\specialreq{SNAP} % To highlight potential bright object violations %\specialreq{SAFTSNP} % Target Type (Required) % %\targtype{A} \targtype{B} %\targtype{C} %\targtype{D} % Desired integration time, in seconds (per visit). For SAFTSNPs, enter % 2000 sec here. For short science observations enter time needed to % achieve listed S/N. See Phase 1 Proposal Instructions for more info. \integrationtime{10000} % (Required) %--------------------------------------------------------------------- % Repeat the above information as needed for each target/observation. \end{observations} \end{document} Note: Additional Examples will be made available on the FUSE JHU Science Center Web page, URL http://fuse.pha.jhu.edu. Appendix A: FUSE Target Naming Conventions< The following is a modified version of the target naming conventions used by the Space Telescope Science Institute for HST proposals. FUSE will use the procedures outlined below to standardize target names in FUSE proposals and in the FUSE archive. Prospective proposers and archival researchers will use these names to determine whether FUSE has observed a particular object. Your adherance to these rules will assist in making the archive more useful for everyone. We thank you in advance for your efforts in this regard. The following conventions must be followed in naming targets: A new target name must be defined for each (celestial) target. For example, for several pointings within a galaxy, one might define target names like NGC4486-NUC, NGC4486-JET, NGC4486-POS1, and NGC4486-POS2. The maximum allowable length of a target name is 30 characters. No blanks are permitted in target names. Blanks between a letter and a numeral must besuppressed (e.g., HD140283, NGC4378), but a hyphen (and not an underscore) must replaceblanks between two letters or two numerals (e.g.