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Athena MOCK OBSERVATION ASST PLAN Title : Athena: Mock Observing Plan Prepared by : Jan-Willem den Herder with inputs from the Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 1 of 26 Date : : Date : PA agreed by : Date : Authorised by : Date : Athena Science Study Team, the Athena science working groups, Jelle de Plaa, Arne Rau, Francois Pajot Checked by Distribution Athena Science Study Team Massimo Cappi Thomas Reiprich Mark Ayre Dave Lumb Ivo Fereira Arne Rau Jelle de Plaa Francois Pajot Jean-Michel Mesagner 15 September 2015 Athena ASST MOCK OBSERVATION PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 2 of 26 Table of contents Abbreviations and acronyms ....................................................................................................... 3 Applicable Documents ................................................................................................................. 3 Reference Documents ................................................................................................................. 3 Document changes...................................................................................................................... 4 1 Introduction ......................................................................................................................... 6 2 Mock Observation Plan .......................................................................................................... 8 3 Summary ............................................................................................................................ 14 App A. Mock Observation Plan: list of entries ........................................................................... 18 App B. Overview of changes in the MOP ................................................................................... 20 App C. Source intensities of GRBs ............................................................................................ 23 App D. count rate estimates .................................................................................................... 24 In order to update the table, click right on a table item and select “Update Field” followed by “Update entire table”. Delete this text of course. Athena Doc. no. : SRON-ATH-PL-2014-001 MOCK OBSERVATION ASST PLAN Issue : 3.0 Date : 15 September 2015 Cat : Page : 3 of 26 Abbreviations and acronyms ASIE Athena Science Impact Exercise MOP Mock Observing Plan TBD To be Determined TOO Target of Opportunity WFI Wide Field Imager XIFU X-ray Integral Field Unit Applicable Documents [AD#] Doc. Reference Issue Title [AD1] Strawman_obsplan_athena V3.0 Excel table with mock observation plan Reference Documents [RD#] Doc. Reference Issue Title [RD1] 2013arXiv1306.2307N June 2013 The Hot and Energetic Universe: A White Paper presenting the science theme motivating the Athena+ mission and all references to the supporting white papers [RD2] n/a April 2014 Athena: the Advanced Telescope for High Energy [RD3] SRE-S/ATH/2015/01 Version 1.4 Athena Science Requirements Document [RD4] ASIE_final.pdf 15 May 2015 Athena Science Impact Exercise [RD5] n/a Draft v1.0, 15 Athena X-ray Stray Light Impact Astrophysics (mission proposal to ESA) June 2016 Athena ASST MOCK OBSERVATION PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 4 of 26 Document changes Version Page changes 0.1 All Initial version 0.3 Updated tables Further information from the various working groups was collected. Key input has been: - additional 18 50 ks observations on nearby clusters to map the background 1.0 Updated update onb SNR observations See change log in excel file for changes: corresponding - harmonized inputs excel table - added fluxes in 2-10 keV range for relevant sources - added a few plots with distribution of sources over the sky - included stellar end points (overlooked in previous versions) - started to match targets to numbered science goals and not only to white paper 1.1 1.3 8,9 - updated plots - added appendix with source intensities of GRBs Version 1.2 was skipped to be able to use the same version number for this document and for the corresponding excel table. Changes include: - introduced a new section 2 with a summary of science goals and re-numbered the next sections - added 25 Ms to the core program for discovery space of a mission in 2028 - implemented the new split between ‘accretion physics’ which is part of the energetic universe together with Sgr A* and ‘end points of stellar evolution’ which remain part of the observatory science - added the average source intensity and allow for checking of total number of observations above certain average source intensity per instrument - added unique reference to science goals (which are not identical to the science goals of the SciRD but are a split between the different topics. And changes in the MOP due to changes in the Science Requirements: - large scale turbulence in clusters (1.1.c) will be determined for 10 regular and 10 irregular clusters. The 10 regular can be the same sample as needed for the metl distribution in the core of 12 clusters (1.2.a) - The AGN ripples are now for 25 clusters but with a longer Athena ASST Version Page MOCK OBSERVATION PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 5 of 26 changes exposure time - The radio galaxy energy needs 90 systems in order to cover the full luminosity ranges and source size ranges 2.0 All Following the Athena Science Impact Exercise (see RDx) the science requirements were updated. Especially the sample sizes were harmonized and more clearly specified. This resulted for the Athena as proposed mission in an updated Mock Observing Plan (version 2.0). in addition some further refinements were added such as source size and countrates. 3.0 Major changes included: - completion of the count rate estimates - revised survey strategy taking into account the fact that significant more time is needed to compensate for the expected lack of a separate straylight baffle - increase of the available time for observations not mandatory to meet the core science objectives. A major change is to use the survey for the cluster entropy (9 Ms) also for the survey. This requires proper handling of the data rights in the SMP as each observation has multiple usage. - Updated the justification for count rate estimates including specification of total data rates for a given observation - Included a fiueld indicating (tentatively) whether or not a observation is background sensitive Relevant changes are marked in red (will be changed to black with the next version) Athena MOCK OBSERVATION ASST 1 PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 6 of 26 Introduction At the time of the preparations of the Athena mission proposal (see RD2) a mock observation plan (version 1.1) was put together and it was verified that in a reasonable mission life time (5 years) the science could be completed with the proposed mission. It should be noted that this assessment was carried out for the baseline mission configuration as given in the mission proposal: angular resolution: 5 arcsec effective area at 1 keV of the optics of 2.1 m2 vignetting corresponding to 3 mm rib spacing Field of view of the WFI 40 x 40 arcmin Field of view and resolution of the X-IFU 5 of arcmin (diameter) and 2.5 eV at 6 keV Following the white paper and the mission proposal two major changes have been implemented in different versions of the MOP: as part of the comparison between the CDF configuration with an area of 1.4 m 2 and the mission as proposed (2 m2) the science requirements were updated and re-grouped. The MOP has been updated accordingly (version 1.4) but this version has not been distributed. This activity was carried out by the end of 2014 but only presented at the ASST meeting. Following the request of the ESA executive this exercise was repeated in a more rigorous way under the name of the Athena Science Impact Exercise (ASIE, ref [RD4]) where the differences between the two configurations were more precisely defined (e.g. same rib spacing for both cases and detailed responses were prepared). Parallel to this exercise the team also updated the science requirements and further refined some of the science objectives (unfortunately this makes it harder to follow the evolution of the MOP as the subtotals are not really comparable). In addition the needed sample sizes were reviewed and updated to be more homogenous (10 objects for a bin in the data space, 25 objects to understand an distribution). The corresponding MOP which was used for the ASIE exercise is version 1.7. As not all observing details were finalized at that stage the reference version for the ASIE exercise is version 2.0 (minor differences exist with version 1.7 but these do not affect the conclusions of the ASIE exercise). It should be noted, however, that following the review by ESA of the ASIE report, additional changes have been requested which were not yet been implemented in version 2.0. Some of the sample sizes will be cross-checked as the samples in version 2.0 are not fully consistent. More importantly the survey strategy was modified from 4x1Ms + 3x700 ks + 9x450 ks + 230x80ks into 4x1Ms + 3x700 ks+10X600ks+299*80ks to compensate for the lack of a separate straylight baffle for the optics. In addition wide field imaging observations for some specific science goals (90 100 ks observations for the cluster entropy (R-SCI-OBJ-121) and 8 for bright local AGN (R-SCIOBJ-241) can also serve as part of the wide survey of 299 x80 ks. Hence 118 observations of the wide field survey have been classified as B (not mandatory for the core science). This had a secondary possitve effect that the fraction of observation time mandatory to meet the core science objectives reduced from 80% to 74% (in line with the recommendation of the Astronomy Working Group) leaving a good part for discovery science and observatory science. Athena ASST MOCK OBSERVATION PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 7 of 26 In parallel to these major changes we have also added some information to the MOP including source intensity, source size, TM rates etc. It is also obvious that the actual observing plan of Athena, as will be decided by the time of the launch by the time allocation committee, will differ from the current plan. Nevertheless the current plan can be used for the purpose of mission design. Athena MOCK OBSERVATION ASST 2 PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 8 of 26 Mock Observation Plan In this section we summarize the science goals as given in [RD3] and the required observations as given in the straw man observation plan [AD1]. For the different science objectives a representative set of observations is listed in the MOP. The relevant information includes the coordinates or the sources, the instrument, the total required observing time and a reference to the science goals. In Table 2-1 the corresponding information is summarized. In this table we neglect that a number of sources is listed twice for different science goals. However, this effect is modest (2.2 Ms in total). For reference the evolution of the observing times between the mission proposal and version 2.0 is given in appendix B. To help the reader to digest the richness of the observation plan, but also to see many interrelations, some general comments can be made: wide field survey: This survey is optimized on different depths and covers 52,7 deg2 to a depth of 7.2 10-17 erg/cm2/s corresponding to 299 pointings of 80 ks with the WFI combined with 2.4 deg 2 to a depth of 2.4 10-17 erg/cm2/s corresponding to 3 observations of 700 ks and 10 of 600 ks supplemented by 1 deg 2 very deep survey (4 x 1 Ms). The integration times and number of observations account for the higher X-ray straylight than was originally assumed at the time of the mission proposal. This survey is multi purpose and covers SCIOBJ-111, 211, 221 and 224. The fields which are selected include the COSMOS field, the Extended CDFS the XXL Northern (LSS) field, ELAIDS-S1, DEEP2-23h, the North Ecliptic pole and the XXL Southern (BCS) field. At time of the launch different fields might be selected but the number of observations will not be random over the sky. Wide field images for selected science objectives: some of the Wide Field Images for selected science objectives will also be used for the survey. For these (and other) observations the science management plan should address the data rights (which can be shared between different groups). The relevant science objectives are the ‘cluster entropy evolution’ (R-SCIOBJ-121) and ‘AGN reverberation mapping’ (R-SCIOBJ-241). GRBs and AGNs as backlight for WHIM: Detection of the WHIM can de done against bright AGNs or against bright GRBs provided that, following an external trigger, the X-IFU can observe the afterglow fast enough that the GRB is sufficiently bright (mCrab level). In addition, some extra measurements are included based on our current knowledge (including the measurement of the correlation function in the COSMOS field). It should be noted, however, that not all these observations are required to achieve the science objective (but the science can clearly benefit from these measurements). Clearly this follow up of the GRBs also requires a fair Field of Regard as the total number of expected GRBs/year is limited). About a third of the GRBs will be at high redshift (z>7) allowing the study of the formation of the earliest stars (POP III) (different SCIOBJ 261). On top of that for selected detections with GRBs, extended observations to measure the WHIM in emission are also included (SCI-OBJ 242). Target of Opportunities: Target of opportunity obervations are critical to the Athena science case. As such there is a well defined science requirements (4 hours after an external trigger Athena should be on target and able to observe the events with the X-IFU). The relevant ToOs are high redshift GRBs, Athena MOCK OBSERVATION ASST PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 9 of 26 other GRBs as backlight for the WHIM, TDE and supernovae. With a total of about 2 ToOs per month it is estimated that the science goals of the mission can be achieved. In reality the number could be higher if this is scientifically justified (and may then go at the expense of additional consuma bles and hence total mission duration) Collect statistical relevant sample of a class of objects: Many of the science goals are not achieved by single observations but require a sufficiently dense sample of sources grouped in relevant parameters (luminosity, size, redshift). As reference we assume a 5 detection per bin. This is justified in the SciRD [RD 3]. In other cases a class of events should be collected which has been set at 25 objects. This explains, for example the rather large programs for determining the evolution of the injection of entropy for clusters and the evolution of metal production in clusters (4 redshift bins and 3 mass bins result each already in 12 Ms). Background fields: limited time has been reserved for a deep exposure for a background field of the WFI and of the X-IFU. In the current plan we took one single 1 Ms observation for each of the instruments, corresponding also to the longest and deepest observations planned for these instruments. Observatory science: in the current plan science which is not part of the science objectives for the Hot and Energetic Universe, but which can already be defined in detail, is listed as observatory science. This helps in defining an optimal observing strategy and distribution of the sources over the sky. Discovery science: for a mission to be launched in more than a decade in the future it is appropriate to reserve time for science which we cannot currently imagine. This is called discovery science. Assuming all observations are carried out without multiple use of a given pointing, this time is limited to 7.5 Ms which is too low. Taking into account the multiple use of Wide Field Images for additional science objectives, this fraction can be increased to 19.5 Ms for a 5 year mission, neglecting specific sources which serve more than 1 science objective (3 Ms in total). Taking into account the this optimization, 74% of the observing time is required to perform the observations mandatory for the core science and 26% for observatory and discovery time. Clearly this does not exclude that in the future time allocation committees will assign more time to this category and less to other areas. Calibration time: the total estimated calibration time is 5% (6 Ms for a 5 year mission). Of this about half can be performed when the other instrument is observing (e.g. variations in particle background) and the other half will required dedicated pointings of calibration sources (e.g. CTI or contamination) Athena OBSERVATION ASST Table 2-1 Doc. no. : SRON-ATH-PL-2014-001 MOCK PLAN Issue : 3.0 Date : 15 September 2015 Cat : Page : 10 of 26 Overview of Mock Observation plan (sub-totals are given in orange fields). Instrument, sample size and the total observing time is listed. In the last column we list the mandatory observing time taking into account multiple usage of relevant observations (in the survey) or secondary goals for a given science objective Science objective survey Hot Universe R-SCIOBJ-111 First groups R-SCIOBJ-112 Cluster bulk motions and turbulence R-SCIOBJ-121 Cluster entropy profile evolution R-SCIOBJ-122 Cluster chemical evolution R-SCIOBJ-131 Physics of cluster feedback R-SCIOBJ-132 Feedback induced cluster ripples R-SCIOBJ-133 Heating/cooling balance in cluster feedback R-SCIOBJ-134 Shock speeds of radio lobes in clusters R-SCIOBJ-141 Missing baryons R-SCIOBJ-142 WHIM in emission Short description large area Instru ment WFI Sample size modest area deep observations WFI WFI 299 x 80 ks but 98 observed as part of other science objectives (see text) 3 x 700 ks + 10 x 600 ks 4 x 1 Ms 25 galaxy groups with gas temperature at z>2 to investigate L-T relation Kinetic energy dissipated from gravitational assembly in 10 regular & 10 irregular galaxy clusters in the nearby Universe Cosmic history of the injection of entropy in cluster hot gas at 0<z<2. Investigate 10 clusters in each of 4 redshift bins and 3 mass bins (total 120 clusters) Metal production and dispersal in cluster hot gas out to z=2. Observe 10 local clusters and 10 clusters per redshift bin per mass bin out to z~2. Total 100 clusters. Bulk motions in 25 cluster cores with AGN, 10 of them mapped in detail to explore microphysics WFI 50% of wide survey X-IFU Mosaic of 10 irregular clusters (regular clusters from 122) WFI Detection of ripples in cluster gas created by AGN jet activity, in a sample of 25 clusters Heating-cooling balance in hot gas of 10 cluster cooling cores MOP total MOP mandatory 23,92 16,08 8,10 4,00 36,02 8,10 4,00 28,18 survey survey 5,00 5,00 30 regular clusters nearby and 90 clusters (100 ks each) for z>0.5 12,00 12,00 X-IFU 30 regular clusters nearby and 90 clusters (100 ks each) for z>0.5 12,00 12,00 X-IFU 3,25 3,25 WFI 25 cluster cores and 10 cluster outskirts (4 observations each), 10 additional specified but not core science 25 clusters 1,25 1,25 X-IFU 10 clusters 0,50 0,50 Shock speeds of expanding radio lobes in 10 clusters around radio galaxies for 2 redshift and 2 radio power bins Detect 200 WHIM filaments in absorption, 150 towards BL Lacs and 50 towards bright GRB afterglows. Determine metal abundances from emission lines in targeted regions WFI 40 clusters in total (originally 60 were proposed 2,00 2,00 X-IFU Cosmos field mapping 2,00 0,00 Bridges sculpture 1,80 1,20 25 AGN 5,26 5,26 Detect emission of WHIM filaments associated with systems detected in absorption detected against 15 GRB afterglows subtotal Hot Universe X-IFU 50 GRBs (+follow up) 15 systems from R-SCIOBJ-141, 200 ks each 2,60 3,00 2,50 3,00 50,66 47,96 sum of survey Athena ASST Doc. no. : SRON-ATH-PL-2014-001 MOCK OBSERVATION PLAN Issue : 3.0 Date : 15 September 2015 Cat : Page : 11 of 26 Energetic Universe R-SCIOBJ-211 High redshift SMBH R-SCIOBJ-221 Complete AGN census R-SCIOBJ-222 Census of AGN outflows at z=1-4 R-SCIOBJ-223 Mechanical energy of AGN outflows at z=1-7 R-SCIOBJ-224 Ultra fast outflows at z=1-4 R-SCIOBJ-231 AGN outflows in the local Universe R-SCIOBJ-232 Feedback in local AGN and star forming regions R-SCIOBJ-241 AGN reverberation mapping R-SCIOBJ-242 AGN spin census R-SCIOBJ-251 GBH and NS spins and winds R-SCIOBJ-252 ULXs and SgrA* R-SCIOBJ-261 High redshift GRBs R-SCIOBJ-262 TDE Detect 10 AGN with 1043.0 < Lx<1043.5 erg/s at z=6-8 and 10 AGN with1044.0 < Lx<1044.5 erg/s at z=8-10. Constrain SMBH seeds. Spectral characterization of at least 10 Compton-Thick AGN with 1044.4<Lx<1044.9 erg/s per unit z at z~3. Map obscured AGN/galaxy coevolution. Detect at least 10 warm absorbers in AGN with 1044<Lx<1044.5 at z=1-4 WFI Wide and intermediate survey Survey survey WFI Deep survey Survey survey WFI Wide survey Survey survey Measure the mechanical energy of outflows in luminous AGN at z=1-3, 10 per 3 luminosity bins and per 2 redshift bin of z=1 . X-IFU 60 observations 3,20 3,20 Frequency and mechanical energy of UFOs at z=1-4 WFI Wide survey Survey survey Wind energetics in 25 nearby AGN out of 70. Wind launch physics from time resolved spectroscopy of 10 AGN. X-IFU 70 observations of 50 ks + 3,50 ,50 1,00 1,00 Gas, metal and energy output from AGN and Starbursts in 25 (U)LIRGs with a variety of AGN/Starburst ratios X-IFU 10 AGNs of 10x10 ks observations each, spread over time 1,69 1,69 Reverberation mapping of 8 bright local AGN with established lags. WFI Only 8 sources known 1,70 1,70 Spin distribution (histogram) of 30 nearby SMBH X-IFU 42 objects to get 30 objects 3,72 3,72 WFI 10 GBH and 10 NS with WFI (X-IFU feasible but takes more time) 2,00 2,00 X-IFU 2 x 10 x 2 ks 0,40 0,40 X-IFU 30 sources 1,50 1,50 and monitor of the SgrA* Probe ISM of z>7 galaxies by ToO observations of 25 GRB afterglows X-IFU 1 observation 25 GRBs with 50 ks within 4 hours 0,15 1,25 0,15 1,25 Probe 10 TDEs by ToO observations. X-IFU 10 TDE (X-IFU) + follow up (WFI) 1.20 1,00 21,31 21.11 a) Measure spins of 10 Galactic BHs and 10 NS through various methods and probe their accretion geometry and jet properties through reverberation mapping. (b) Measure winds in the same 10 Galactic BHs and 10 NS. Accretion properties of 3 luminosity bins of 10 ULXs subtotal energetic Universe Athena Doc. no. : SRON-ATH-PL-2014-001 MOCK OBSERVATION ASST PLAN Observatory science R-SCIOBJ-311 Auroral and exosphere X-ray Planetary Xemissions of solar system bodies ray (planets and moons) and cometary Spectroscopy tails & their interaction with Solar Wind. R-SCIOBJ-312 Effects of stellar magnetic activity of 6 Stellar activity exo-planets through repeated in exo-planet observations through their orbits systems R-SCIOBJ-322 Wind interactions in binaries through Colliding winds phase-resolved spectroscopy in 10 in binaries massive binaries. Issue : 3.0 Date : 15 September 2015 Cat : Page : 12 of 26 WFI X-IFU 12 solar system bodies including comets 0,64 X-IFU 6 known objects, at time of mission it might be more 0,95 X-IFU WFI 13 objects (10 X-IFU, 3 WFI) 1,80 R-SCIOBJ-323 Magneticspheri c accretion in low mass binaries Magnetospheric phenomena and/or accretion in nearby field M Stars, latetype PMS stars and BDs, and magnetospheric accretion phenomena and circumstellar disk interactions in YSOs in selected nearby SFRs. WFI, X-IFU Magnetospheric accretion in 18 young low-mass stars and brown dwarfs 1,04 R-SCIOBJ-324 Magnetic activity in ultra-cool dwars Magnetic activity in ultra-cool dwarf stars X-IFU Observe sample of 4 objects 0,17 R-SCIOBJ-325 Mass loss in massive stars Characterize the mass-loss and winds in a sample of early type stars and in HMXBs. X-IFU WFI 8 objects to characterize winds 0,61 X-IFU WFI 30 objects 1,57 7 LMBXs, 2 interesting milliesecond pulsars will be done by Nicer and are not included 10 objects selected 0,45 Measure the X-ray spectra of selected OB associations (each containing at least 10 massive stars) in 3 different Local Group galaxies with different metallicities. R-SCIOBJ-331 EOS of ultradense matter Equation of state of dense matter from observations of LMXBs WFI R-SCIOBJ-333 Masses of accreting white dwarfs R-SCIOBJ-334 magnetars S-SCIOBJ-335 PWN Determine M/R ratio of accreting white dwarfs WFI, X-IFU Characterize geometry of magnetars and XDINs Constrain particle acceleration by the study of PWN WFI X-IFU WFI X-IFU 10 systems selected 0,50 7 objects 0,80 S-SCIOBJ-336 Novae Observe 3 nova going off during Athena mission X-IFU 10 observed with 6 x 5 ks each 0,30 10 plenatary nebulae 0,38 and 10 planetary nebula S-SCIOBJ-337 double degenerate binaries R-SCIOBJ-338 SN R-SCIOBJ-341 Chemistry of cold ISM R-SCIOBJ-342 0,68 Observe double degenerate systems and on type 1A supernova at distance < 25 Mpc X-IFU 9 systems 0,39 BH birth through 10 SN X-IFU 10 SN 0,50 Chemical composition of cold ISM through absorption spectroscopy X-IFU WFI 8 objects for 341 and 342 0,57 Dust models and particle distribution X-IFU 3 objects for 342 and 0,09 Athena OBSERVATION ASST Dust scattering haloes R-SCIOBJ-343 Physics of the warm and hot ISM R-SCIOBJ-344 Mapping of SNR R-SCIOBJ-351 SgrA* Facility time R-SCIOBJ-399 Discovery science calibrations background Doc. no. : SRON-ATH-PL-2014-001 MOCK PLAN through scattering halos Issue : 3.0 Date : 15 September 2015 Cat : Page : 13 of 26 343 Characterize warm and hot ISM in the Galaxy and nearby galaxies X-IFU 3 objects only for 343 0,60 3D mapping of SNR from SN1a and core-collapse SN X-IFU Snap shots of distinct features in 8 SNR 1.00 Characterization of the quiescent diffuse emission from SgrA*, the nonthermal flares and the X-ray reflection nebulae surrounding the Galactic Centre WFI 5 observations to map environment 0,25 13,28 13,28 7,50 19,70) 3,34 3,34 2,00 2,00 total 134,12 133,97 MOP without duplications) 5 year mission (85%) [Ms] 131,19 134,00 134,00 0,53 0,58 Athena should be able to respond to scientific challenges triggered by new developments, including new multiwavelength or other messenger observations 5% of which half is when instrument is not in the focus observatory + discovery + background [%] X-IFU observing fraction X-IFU WFI Time which is not yet assigned and together with the observatory science this is not required to meet the core science goals as defined in the proposal 17% 26% The MOP allows making various selections that help to define the mission requirements. For example one can determine the total mission duration mandatory for the core science, the distribution of the sources over the sky, the division in observing time between the XIFU and the WFI. As detailed information is given about all known source positions, duplications in the observing plan can be avoided as well. In the current excel sheet these sources are included but a field is added to indicate if the source is already observed as part of another program. MOCK Athena OBSERVATION ASST 3 PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 14 of 26 Summary Based on this mock observing plan the following conclusions can be drawn: - The total observing time mandatory to realize the Hot and Energetic Universe science described in the white paper is 99 Ms corresponding to 72% of 5 years observing time (assuming a observing efficiency of 85% and 2% effective observing time for calibrations). For the Observatory science and the discovery science 35 Ms (26%) of the time is allocated but it should be recognized that not all observations listed under the Hot and Energetic Universe are required to realize the mission goals: Table 2 Overview of the observing time (the percentages are rounded and do not sum to 100) Category Mandatory Total (includes Mandatory [Ms] multiple used [% of total observations) time] [Ms] Survey (but about 10 Ms is accounted as part 26,6 36,0 20 Hot Universe 48,0 50,7 36 Energetic Universe (but some science drives 21,1 21,3 16 Observatory science1) 13,3 13,3 9 Discovery science 19,5 19,5 15 2,0 2,0 1 3,3 3,3 of the Hot Universe or Energetic Universe and are also part of the survey) the survey) 1) Background1) Calibration Total observing time observing time for specific targets relevant to 2 134,1 100 2,9 2 different science objectives 1) Observatory science, discovery science and background observations are not mandatory for the core science but are listed here to give a full overview of the expected observing plan. For the Observatory science targets have been identified whereas for the discovery science this is not done. A 5 year mission with an ambitious 85% observing efficiency and a 2 m2 effective area with 5 arcsec resolution enables the science selected in the white paper. To realize this it is also required that by selection of an optimal orbit and the optimization of the instruments, the fraction of not usable data due to high background is small compared to XMM-Newton (70%). - the relative split between mandatory observations with the XIFU and the WFI is 58% to 42%. With a typical regeneration time of the XIFU of less than 30% one may expect that this regeneration time of the XIFU will not drive the mission lifetime or observing schedule. - The number of observations exceeding 100 ks is limited. In general these observations can be interrupted for a shorter period for unloading the reaction wheels but much less than 50 ks Athena MOCK OBSERVATION ASST PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 15 of 26 uninterrupted time has the risk to create observing inefficiencies. The longer observations (also with the X-IFU) can be split in multiple exposures without problems. - The total number of transient events for which a fast slewing is needed is about 100 (TBC) over the 5 year mission duration (typically 1 per every two weeks but the distribution will be random over time). - The distribution of the known sources is shown in Figure 3-1 and Figure 3-2. Clearly the hot and Energetic Universe science has a preference for targets outside the Galactic Plane. This is representing the preference for these targets for a number of science topics (e.g. cluster redshift study, deep sky observations). The not yet known sources (GRB, SN, TDE) will be distributed uniformly over the sky except for the unknown clusters which are assumed to be at |b| > 10 o. Figure 3-1 Distribution of sources (WFI and XIFU separate) over the sky. The WFI surveys can be seen as set of connected red dots. Athena ASST Figure 3-2 MOCK OBSERVATION PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 16 of 26 Distribution of sources (required (A) and desirable (B) for the Hot and Energetic and required (C) and desirable (C) for the observatory science (D)). Note that this division is not yet made!. Clearly visible is the set of Galactic compact objects that are part of the observatory science. - In addition we can provide the total integrated exposure time over the sky for all the science given in the corresponding mock observation plan. This is given in Figure 3-3. Athena ASST MOCK OBSERVATION PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 17 of 26 Figure 3-3 Total integrated exposure time over the mission duration to perform all science given in the white papers Athena MOCK OBSERVATION ASST PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 18 of 26 App A. Mock Observation Plan: list of entries In the mock observation plan we list the following information (in italic key information, other columns are supporting columns for statistical purpose only): Source name Science group (0 = observatory, 1 = finding early groups, 2 = cluster velocity etc, see bottom of the table) Core science class (>1 required as it is class A, <0 important but not required (class B) duplication (N if it occurs only once, Y if it appears in another program with a longer observation and the same instrument, this is a manual check and a few cases may have been overlooked (or sources has two different names such as Sersic159-03 and S1101) Source classification (could also be survey) RA (for most raster scans different positions are given with the exception of the 1 year survey for the formation and growth of supermassive black holes (group 13) Dec l b number of observations exposure time per observation [ks] Total observing time (ks): (number of observations x exposure time per observation) Total observing time corrected for duplications (the longest observation of a source/instrument combination is used) Class: Can be used to specify which targets are mandatory for a minimum mission success and which are ‘good to have’ but not critical for the mission success. A is mandatory to achieve core science requirements, B good to have to accomplish the core science goals, C mandatory to achieve the observatory science and D good to have to accomplish the observatory science. This column is currently not used and not correctly applied but is left in the excel sheet for future use. ToO (NO or, if yes identify the type with the following code: VF(<4 hrs), F(4-24 hrs), N(1-3 days), S(3days-7 days), VS(1-3 weeks) Continuous: Y if it is mandatory not to interrupt the measurement (this column is not consistently filled). It should be noted that many of the > 50ks observations can be split into multiple observations. In general it is, however, recommended not to separate them in time over more than a few weeks as the science objective requires the full data to be completed. Instrument: WFI or XIFU Instrument mode: for WFI and X-IFU separately Source intensity (either given by the ASST or by ESA (= Dave Lumb)) used to calculate the TM rates Background critical: indication which observations depend critically on typical background variations (factor 2 or 3). In general as rule bright point sources and faint sources or extended sources for which the spectrum < 2 keV contains the scientific information are not critical dependent on the background. Note that this is indicative only (in the MOP) and real cases can be different TM rates: model, scaling to kBit/s, approximate TM rate and typical data volume (rate x observing time) T_observation for X-IFU > limit_XIFU and T_observation for WFI > limit_WFI: observation time if the source intensity is above the limit specified in the bottom of the table (now 10 and 1000 mCrab). The Athena MOCK OBSERVATION ASST PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 19 of 26 average intensity of the source is given in the 2 – 10 keV range which excludes variations in the source intensity (can be significant for AGNs) Source intensity: average source intensity from the RXTE mission in the 2 – 10 keV region Source size: for clusters the R200 value and an assessment whether it is regular or irregular Science goals: number science goal, note that some observations support more than a single science goal and this can be seen in either more than a single value in this column or a source may appear twice with the relevant switch (duplication) set to yes. Science goal: reference to the numbers science goals in the mission proposal Science topic (this one and the next are not checked on consistency) Science subtopic Synergy with other programs: identify other programs/topics that can use the specific target, thus allowing to optimize the observing plan Key measurement: identify the main observable/parameter of the observation Justification and comment: on the required exposure time (plus any other comment you deem relevant for that specific target Observing strategy: summarize the observing strategy for each science topic/subtopic Doc. no. : SRON-ATH-PL-2014-001 MOCK Athena OBSERVATION ASST PLAN Issue : 3.0 Date : 15 September 2015 Cat : Page : 20 of 26 App B. Overview of changes in the MOP In the table below we present the changes in the MOP since its first released version (1.1). Version 1.4 was never completed but was used to assess the differences between the mission as proposed and the mission as studied in the ESA CDF activity (December 2014). Following this the Athena Science Study team was requested to study the differences in more detail (ASIE) and version 1.7 was used for this exercise. However, the deadline of this exercise (May 2015) and the availability did not allow the have a full MOP consistent with the updated science goals. This has been realized in version 2.0. Following the Mission Consolidation Review and the recommendations by the Astronomy Working Group version 3.0 of the MOP was generated. By using the observations for the cluster entropy (ER-SCIOBJ-121) also for the survey, the fraction of not allocated time for core science was increased. Also the survey strategy was modified somewhat to take into account the recommendation of the ASST at its 10 th meeting not to have an X-ray baffle as part of the baseline design). Finally count rate estimates were added. Table B.1 Overview of Mock Observation plan. Science objective survey Short description MOP 2 28,54 14,9 5,6 4,0 24,50 MOP ASIE (1.7) 18,40 6,15 4,00 28,55 18,40 6,15 4,00 28,55 23,92 8,10 4,00 36,02 25 galaxy groups with gas temperature at z>2 to investigate L-T relation Kinetic energy dissipated from gravitational assembly in 10 regular & 10 irregular galaxy clusters Cosmic history of the injection of entropy in cluster hot gas at 0<z<2. Investigate 10 clusters in each one of 4 redshift bins and 3 mass bins (total 120 clusters) Metal production and dispersal in cluster hot gas out to z=2. Observe 10 local clusters (needs mosaicing) and 10 clusters per redshift bin per mass bin out to z~2. Total 100 clusters. Nearby clusters (z< 0.5) Survey Survey survey survey survey 1,60 3,00 2,00 0,00 5,00 9,00 9,00 12,00 12,00 12,00 2,40 1,80 0,00 3,00 3,00 large area modest area deep observations MOP 1.1 MOP 1.4 sum of survey MOP 3 total Hot Universe R-SCIOBJ-111 R-SCIOBJ-112 R-SCIOBJ-121 R-SCIOBJ-122 R-SCIOBJ-131 R-SCIOBJ-132 R-SCIOBJ-133 R-SCIOBJ-134 R-SCIOBJ-141 Clusters z=0.5 – 2.0 9,00 9,00 9,00 9,00 9,00 Mosaic for nearby clusters (also 112) 0,00 0,00 5,00 5,00 See 112 total SCIOBJ 122 11,40 10,80 14,00 17,00 17,00 3,80 3,80 3,75 3,75 3,25 0,98 1,30 1,25 1,25 1,25 0,50 0,50 0,50 0,50 0,50 2,00 4,50 2,00 2,00 2,00 Bulk motions in 25 cluster cores with AGN, 10 of them mapped in detail to explore microphysics in detail Detection of ripples in cluster gas created by AGN jet activity, in a sample of 25 clusters Heating-cooling balance in hot gas of 10 cluster cooling cores Shock speeds of expanding radio lobes in 10 clusters around radio galaxies per 2 redshift and 2 radio power bins Detect 200 WHIM filaments in absorption, 150 towards BLLacs and 50 towards bright GRBs. Determine metal abundances from emission lines Athena ASST MOCK OBSERVATION PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 21 of 26 in targeted regions R-SCIOBJ-142 Cosmos field Bridges and sculptor field AGN GRB follow up 1,20 1,80 5,30 5,00 2,00 1,00 5,00 5,00 2,00 1,80 5,26 2,50 2,00 1,80 5,26 2,60 sum SCI-OBJ 141 13,30 13,00 13,58 11,56 11,66 Detect WHIM filaments in emission associated to absorption detected against 15 GRBs, after they faded away subtotal hot Universe 3,00 3,00 3,00 3,00 3,00 45,58 51,90 52,08 51,06 50,66 Detect 10 AGN 1043.0 < Lx<1043.5 erg/s at z=6-8 and 10 AGN 1044.0 < Lx<1044.5 erg/s at z=8-10. Constrain SMBH seeds. Detect at least 10 Compton-Thick AGN 1044<Lx<1044.5 erg/s per unit z at z~3. Map obscured AGN/galaxy co-evolution. Detect at least 10 warm absorbers in AGN 1044<Lx<1044.5 at z=1-4 Measure the mechanical energy of outflows in luminous AGN at z=1-3, 10 per 3 luminosity bins and per redshift bin. Frequency and mechanical energy of UFOs at z=14 Wind energetics in 30 nearby AGN. Wind launch physics from time-resolved spectroscopy of 10 AGN Gas, metal and energy output from AGN and Starbursts, using 25 (U)LIRGs with a variety of AGN/Starburst ratios Reverberation mapping of 8 bright local AGN survey survey survey survey survey survey survey survey survey survey survey survey survey survey survey 3,00 3,20 3,20 Spin distribution (histogram) of 30 nearby SMBH Measure spins of 8 Galactic BHs through various methods. Winds and jets in 15 BHs. Gain insight on BH birth though observations of 10 Supernovae Accretion geometry around compact sources through reverberation mapping. Study Tidal Disruption Events and SgrA* (no TDEs version 3) Probe ISM of z>7 galaxies by ToO observations of 25 GRB afterglows 10 TDEs (in 252 till version 3) subtotal energetic Universe Energetic Universe R-SCIOBJ-211 R-SCIOBJ-221 R-SCIOBJ-222 R-SCIOBJ-223 R-SCIOBJ-224 R-SCIOBJ-231 R-SCIOBJ-232 R-SCIOBJ-241 R-SCIOBJ-242 R-SCIOBJ-251 R-SCIOBJ-252 R-SCIOBJ-261 R-SCIOBJ-262 6,00 survey survey survey survey survey 3,10 4,50 4,50 4,50 4,50 0.75 2,50 2,20 1,69 1,69 2,38 3,00 1,70 3,80 1,70 3,72 0,00 3,33 2,50 3,70 2,96 3,72 5,00 3,72 2,40 2,05 3,10 3,30 1,60 1,65 2,50 2,50 2,50 2,50 1,25 20,50 23,73 23,86 26,01 1,20 21,31 0,64 0,64 0,64 0,64 0,64 0,95 1,00 0,95 0,95 0,95 4,28 4,38 4,40 4,15 1,80 1,04 1,02 1,04 1,04 1,04 0,17 0,18 0,17 0,17 0,17 - - - - 0,61 Observatory science R-SCIOBJ-311 R-SCIOBJ-312 R-SCIOBJ-322 R-SCIOBJ-323 R-SCIOBJ-324 R-SCIOBJ-325 Atmospheres and exospheres of solar system bodies (planets and moons) and cometary tails & their interaction with Solar Wind. Effects of stellar magnetic activity of 6 exo-planets through repeated observations through their orbits Wind interactions in binaries through phaseresolved spectroscopy in HMXB (30), LMXB (13) and PNe (11). From version 3 only in 10 massive binaries. (moved to 325 in version 3) Magnetospheric accretion in 18 young low-mass stars and brown dwarfs Magnetic activity in 4 ultra-cool dwarf stars Mass loss and winds in early type stars and in HXMBs and selected OB associations 1,57 Athena MOCK OBSERVATION ASST R-SCIOBJ-331 PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 22 of 26 R-SCIOBJ-333 Equation of state of dense matter from observations of 10 neutron stars Characterize fully the mass-loss and winds in 16 massive stars, both isolated and in binary systems. Dropped and combined with 251 Determine M/R ratio of accreting white dwarfs R-SCIOBJ-334 Geometry of magnetars and XDINs - - - - 0,50 R-SCIOBJ-335 PWN (was in 322) - - - - 0,80 R-SCIOBJ-336 3 nova and 10 planetary nebulae - - - - R-SCIOBJ-337 Double degenerate binaries R-SCIOBJ-341 Chemical composition of cold ISM through absorption spectroscopy Dust models and particle distribution through scattering halos Characterize warm and hot ISM in the Galaxy and nearby galaxies 3D mapping of SNR from SN1a and SNcc R-SCIOBJ-332 R-SCIOBJ-342 R-SCIOBJ-343 R-SCIOBJ-344 R-SCIOBJ-399 calibrations background Athena should be able to respond to scientific challenges triggered by new developments, including new multi-wavelength or other messenger observations 5% of which half is when instrument is not in the focus total in relevant documents (version 1.1, blank, ASIE and MOP 2.0 GRB colow up (in MOP but class B already) MOP corrected MOP without duplications) 5 year mission (85%) [Ms] observatory + discovery [%] 0,60 0,60 0,60 0,64 0,45 4,40 1,30 1,25 1,32 0 0,00 0,00 0,54 0,54 0,68 - - - - 0,30 0,38 0,50 0,68 0,68 0,63 0,63 0,58 0,00 0,83 0,95 0,00 0,09 0,90 0,92 0,95 0,82 0,60 1,17 14,83 0,00 1,17 12,62 25,00 1,17 12,33 15,00 1,17 12,10 15,00 1,00 13,28 19,70 0,00 6,00 3,40 3,35 3,35 2,00 2,00 2,00 2,00 2,00 111,45 145,75 137,22 138,07 137,30 138,17 146,12 133,971) 134,03 0,10 138,07 135,19 134,03 20 20 Notes: 1) After correcting for Wide Field Imaging observations which can also be used for the survey (e.g. cluster entropy survey) 131,19 134,03 26 Athena ASST MOCK OBSERVATION PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 23 of 26 App C. Source intensities of GRBs The source intensities of GRBs have been estimated based on the source intensity distribution as observed by Swift (private comm P. O’Brien) 4 hours after the burst onset. This information as been converted into the corresponding 2 – 10 keV range using a spectral slope of -2. This gives one source at a 2 mCrab intensity. MOCK Athena OBSERVATION ASST PLAN Doc. no. : SRON-ATH-PL-2014-001 Issue : 3.0 Date : 15 September 2015 Cat : Page : 24 of 26 App D. Count rate estimates In this section we report the estimated count rates based on private communication with the two instrument teams. It is assumed that in a later stage this information will be formalized as part of the interface documentation for the instruments. Wide Field Imager There has been an initial estimate for the countrates in the WFI and these are given as reference (WFI-MPEANA-0000-Data-Rate, IDI, 19/06/2015). The WFI countrates are based on simulations using the SIXTE package and the main steps are listed below (numbers approximately correct): - estimates are made for 4 typical cases: Chandra Deep Field South, the Galactic Center, CasA and a Crab-like source - For each event the multiplicity of the event is simulated (singles, doubles, etc). This varies typically between 1.3 (CDFS) to 1.7 (other fields) - number of bits per pixel is 41 for the fast detector and 42 for the large detector - data compression of a factor 2.3 is assumed based on the simulations for the Crab data, for all other no data compression is assumed. - A background component is assumed based on the instrument requirement of 5 10 -3 cnts/cm2/s/keV - a 5 sigma threshold on the pixel is assumed for frames corresponding to 5.1 kbit/s for the fast detector and 12,7 kbit/s for the large detector - a housekeeping allocation of 4.3 kbit/s is included - a 20% margin is applied to the calculated data rates - Charge deposited by MIPs will be rejected onboard Table 3 Overview of simulated countrates for the WFI (data rates include compression (Crab) and a 20% margin and 1024 bits/kbit) Field CDFS GC Countrate Data rate Varia- [events/s] [kbit/sec] bility Typical sources and science objectives in MOP 40 40 1 Survey (R-SCIOBJ-111, 211, 222, 224) 208 53 1 Galactic center (R-SCIOBJ-351), planets (331) 2 Cluster entropy (R-SCIOBJ-121), cluster feedback (132, 134), reverberation (241), colliding winds in binaries (322), magnetic accretion (323), mass loss in massive stars CasA 10.861 913 Crab 121.494 4200 Not used for WFI varying Accretion geometry 15 GBH and 10 NS (251), Equation of State (331), M/R of accreting white dwarfs (333) background 37 1 WFI background measurement 0,3 1 Not used in MOP large background Athena Doc. no. : SRON-ATH-PL-2014-001 MOCK OBSERVATION ASST PLAN Issue : 3.0 Date : 15 September 2015 Cat : Page : 25 of 26 fast X-ray Integral Field Unit Reference, e-mail from Pajot (dd 18 May 2016) and the attached file ‘2016-05-17 data-budget.xlsx’. This calculation includes the following components: - a source dependent component. An 1 mCrab source corresponds to 95 counts/s but it should be recognized that AGNs af a given average source strength may vary up to a factor a few (5 is taken as a reasonable safe number) - a source independent component which is considered stable but it should be recognized that especially for the background component this is not correct (but this is taken into account in the applied margin). These components are given in Table 4. Table 4 countrate estimates for the X-IFU Component Value Event Margin kbit/s (per size1) [%] (without second) comment header) Source mCrab 64 20 7,3 Scales with source intensity Cryoac rate 40 counts 40 100 3,2 Based on cryoAC analysis, data are transferred to the ground for correlation with the TES particles in TES 22 counts 64 200 4,3 Area of TES is about half of the cryoAC. It is assumed that the particles deposit an energy in the 0.2 – 15 keV range in the TES (is a conservative approach) and cannot be identified onboard Total sky 1 counts background integrated 64 100 0,1 Foreground and Cosmic X-ray background (0,3 counts/s) over array Calibration 2400 40 0 96 events Assumes no data processing onboard except selection of events in lines and a reduced energy grid only accurate around lines. House keeping 10 kbit/s 20 12 Estimate (300 parameters @ I1 Hz, 3000 parameters @ 1/8 Hz Total stable 1) 116 Dominated by number of calibration events Event size includes typically a 20% margin In practice this gives a number of cases for the Mock observing plan taking into account that the instrument has a requirement of 30% throughput for a 1 Crab source. Whether or not this TM rate for the very intense sources is achieved by buffering onboard over more than one telemetry pass or not is not part of the MOP. It Athena ASST Doc. no. : SRON-ATH-PL-2014-001 MOCK OBSERVATION PLAN Issue : 3.0 Date : 15 September 2015 Cat : Page : 26 of 26 should also be noted that in case of long observations of bright sources (e.g. SAX J1747.0-2583) the observation can be split into several separate observations spread over time. Source strength TM rate [kbit/s] comment including overhead (headers etc)1) 1 mCrab 145 Requirement for high-res events 10 mCrab 220 Goal for high res events 50 mCrab 550 100 mCrab 980 300 mCrab (which is the maximum required rate 2650 Requirement for throughput with 30 eV resolution: less bits can be applied per event (requirement is still TBC) 1) The overhead for packing is assumed to be 15%, in the MOP we apply for variable sources typically a factor 5 margin for the source strength