Extragalactic Confusion Limits in Herschel Key Programs Mattia Vaccari & Alberto Franceschini &...
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Extragalactic Confusion Limits Extragalactic Confusion Limits in Herschel Key Programs in Herschel Key Programs Mattia Vaccari & Alberto Franceschini & Giulia Rodighiero & Mattia Vaccari & Alberto Franceschini & Giulia Rodighiero & Stefano Berta Stefano Berta Department of Astronomy - University of Padova Department of Astronomy - University of Padova A) Summary A) Summary ISO, Spitzer & SCUBA counts are used to constrain models of ISO, Spitzer & SCUBA counts are used to constrain models of extragalactic populations extragalactic populations Extragalactic confusion in Herschel bands is estimated using 2 Extragalactic confusion in Herschel bands is estimated using 2 complementary criteria complementary criteria The two approaches respectively measure cell-to-cell fluctuations due The two approaches respectively measure cell-to-cell fluctuations due to unresolved sources and set a maximum number density for resolved to unresolved sources and set a maximum number density for resolved sources sources These two methods provide results which are in good agreement for all These two methods provide results which are in good agreement for all Herschel bands Herschel bands Currently envisaged sensitivities for Herschel KP surveys are Currently envisaged sensitivities for Herschel KP surveys are compared with our predictions and opportunities for Herschel OT compared with our predictions and opportunities for Herschel OT extragalactic KP surveys are outlined extragalactic KP surveys are outlined Mattia Vaccari Mattia Vaccari mattia@mattiavaccari .net www.mattiavaccari.net E) “Fluctuations” vs. “Counts” Confusion Limits E) “Fluctuations” vs. “Counts” Confusion Limits 3 3 “Fluctuations” are very close to “Counts” 10 bps for PACS “Fluctuations” are very close to “Counts” 10 bps for PACS but nearer to 20 bps for SPIRE, due to different count slopes at but nearer to 20 bps for SPIRE, due to different count slopes at and fainter than 10/20 bps levels and fainter than 10/20 bps levels The availability of multi- The availability of multi- data (e.g. MIPS 24 data (e.g. MIPS 24 m for PACS, m for PACS, PACS & SCUBA2 for SPIRE, etc) will be invaluable in linking PACS & SCUBA2 for SPIRE, etc) will be invaluable in linking various wavelength regimes and accurately pin-pointing sources in various wavelength regimes and accurately pin-pointing sources in order to reach down to 10 bps levels in all Herschel bands. order to reach down to 10 bps levels in all Herschel bands. See posters by Franceschini on H-COSMOS and by Dunne & Dunlop on See posters by Franceschini on H-COSMOS and by Dunne & Dunlop on H-SCLS H-SCLS B) Confusion at Long Wavelengths with Herschel B) Confusion at Long Wavelengths with Herschel Confusion sets a major limit to the sensitivity of long- Confusion sets a major limit to the sensitivity of long- extragalactic surveys extragalactic surveys As IRAS first dramatically showed, the FIR/sub-mm sky is very As IRAS first dramatically showed, the FIR/sub-mm sky is very densely populated densely populated ISO & Spitzer & SCUBA confirmed this view providing a wealth of ISO & Spitzer & SCUBA confirmed this view providing a wealth of additional data additional data Great care must be taken in taking stock of current knowledge in Great care must be taken in taking stock of current knowledge in order to predict Herschel confusion limits and thus allow a timely order to predict Herschel confusion limits and thus allow a timely planning of GT & OT KP observations planning of GT & OT KP observations D) Measuring Confusion through “Fluctuations” & D) Measuring Confusion through “Fluctuations” & “Counts” “Counts” “ “ Fluctuations” measure fluctuations in the background due to Fluctuations” measure fluctuations in the background due to unresolved sources [Franceschini et al. 1989 (ApJ, 344) ] and set unresolved sources [Franceschini et al. 1989 (ApJ, 344) ] and set “confusion” at the “confusion” at the 3 3 fluctuation level fluctuation level “ “ Counts” measure source counts and set “confusion” where a maximum Counts” measure source counts and set “confusion” where a maximum number of sources per beam, or rather a minimum number of beams per number of sources per beam, or rather a minimum number of beams per source (bps), is reached [Franceschini et al. 2001 (A&A, 378)] source (bps), is reached [Franceschini et al. 2001 (A&A, 378)] Roughly speaking, while “Fluctuations” follow the trend of counts Roughly speaking, while “Fluctuations” follow the trend of counts fainter than the confusion limit, “Counts” follow the trend at fainter than the confusion limit, “Counts” follow the trend at brighter fluxes than that. The degree of consistency between the two brighter fluxes than that. The degree of consistency between the two depends on the slope of counts at and near this flux limit. depends on the slope of counts at and near this flux limit. F) Recommendations for Herschel GT & OT KP F) Recommendations for Herschel GT & OT KP Planning Planning From a confusion point of view, From a confusion point of view, target sensitivities target sensitivities envisaged in Herschel GT KP surveys appear to be realistic when envisaged in Herschel GT KP surveys appear to be realistic when modeling ISO & Spitzer & SCUBA results. modeling ISO & Spitzer & SCUBA results. Opportunities exist to go deeper (see posters by Franceschini Opportunities exist to go deeper (see posters by Franceschini on H-COSMOS and by Dunne & Dunlop on H-SCLS) and wider (see on H-COSMOS and by Dunne & Dunlop on H-SCLS) and wider (see posters by De Zotti on SPIRE LAS and by Serjeant on H-SASSy) over posters by De Zotti on SPIRE LAS and by Serjeant on H-SASSy) over medium- and large-size areas. medium- and large-size areas. In particular, judging from Spitzer results, reaching the 3 In particular, judging from Spitzer results, reaching the 3 ~ ~ 10 bps levels in all PACS & SPIRE bands over larger areas than 10 bps levels in all PACS & SPIRE bands over larger areas than planned in GT KP surveys appears to be feasible and thus somehow planned in GT KP surveys appears to be feasible and thus somehow mandatory in order to fulfill Herschel’s potential for mandatory in order to fulfill Herschel’s potential for extragalactic surveys. Such deep OT KP surveys should be extragalactic surveys. Such deep OT KP surveys should be undertaken over sky areas where deep Spitzer MIPS 24 undertaken over sky areas where deep Spitzer MIPS 24 m and/or m and/or SCUBA2 coverage is or will soon be available, e.g. within the SCUBA2 coverage is or will soon be available, e.g. within the most popular “Cosmic Windows”. most popular “Cosmic Windows”. Survey-like ultra-deep exploratory efforts should be undertaken Survey-like ultra-deep exploratory efforts should be undertaken Channel Channel PACS1 PACS1 PACS2 PACS2 PACS3 PACS3 SPIRE1 SPIRE1 SPIRE2 SPIRE2 SPIRE3 SPIRE3 m m 70 70 110 110 170 170 250 250 350 350 500 500 Beam FWHM Beam FWHM 4 .74” 4 .74” 6.96” 6.96” 10.76” 10.76” 17.1” 17.1” 24.4” 24.4” 34.6” 34.6” 3 3 [mJy] [mJy] 0.07047 0.07047 1.002 1.002 7.484 7.484 18.12 18.12 22.55 22.55 20.19 20.19 10 bps 10 bps [mJy] [mJy] 0.1100 0.1100 1.263 1.263 7.090 7.090 14.00 14.00 15.23 15.23 13.23 13.23 20 bps 20 bps [mJy] [mJy] 0.3029 0.3029 2.746 2.746 11.82 11.82 20.49 20.49 21.65 21.65 18.31 18.31 30 bps 30 bps [mJy] [mJy] 0.4887 0.4887 4.034 4.034 15.23 15.23 25.40 25.40 26.34 26.34 21.49 21.49 40 bps 40 bps [mJy] [mJy] 0.6656 0.6656 5.110 5.110 18.12 18.12 29.18 29.18 29.93 29.93 24.09 24.09 50 bps 50 bps [mJy] [mJy] 0.8350 0.8350 6.107 6.107 20.45 20.45 32.47 32.47 33.05 33.05 26.18 26.18 C) Modelling ISO, Spitzer & SCUBA Observations C) Modelling ISO, Spitzer & SCUBA Observations Models by Franceschini et al. 2001 (A&A, 378) were updated to account Models by Franceschini et al. 2001 (A&A, 378) were updated to account for intervened reanalyses of ISO 15 for intervened reanalyses of ISO 15 m data and results from Spitzer m data and results from Spitzer MIPS and SCUBA observations MIPS and SCUBA observations Models describe available observables (number counts, z- Models describe available observables (number counts, z- distributions, L-functions, integrated CIRB levels…), in terms of four distributions, L-functions, integrated CIRB levels…), in terms of four populations populations slowly or non-evolving disk galaxies [ slowly or non-evolving disk galaxies [ blue blue dotted lines] dotted lines] type-1 AGNs evolving as shown by UV and X-ray selected quasars & type-1 AGNs evolving as shown by UV and X-ray selected quasars & Seyferts Seyferts [ [ green green long-short dashed lines] long-short dashed lines] moderate-luminosity starbursts with peak emission at z ~ 1 [ moderate-luminosity starbursts with peak emission at z ~ 1 [ cyan cyan dot-dashed lines] dot-dashed lines] ultra-luminous starbursts with peak evolution between z = 2 and z = ultra-luminous starbursts with peak evolution between z = 2 and z = 4 4 [ [ red red long dashed lines] long dashed lines] Name Name Area Area Field Field PACS PACS Time Time SPIRE SPIRE Time Time 70 70 110 110 170 170 250 250 350 350 500 500 - - deg^2 deg^2 - - hr hr hr hr mJy mJy mJy mJy mJy mJy mJy mJy mJy mJy mJy mJy Cluster Cluster s s - - - - 80 80 100 100 - - - - - - - - - - - - Level 1 Level 1 0.04 0.04 GOODS-S GOODS-S 230 230 10 10 + + 30 30 1.0 1.0 1.0 1.0 1.0 1.0 3.3 3.3 4.0 4.0 4.6 4.6 Level 2 Level 2 0.04 0.04 GOODS-N GOODS-N 27 27 10 10 2.0 2.0 2.8 2.8 3.0 3.0 6.7 6.7 8.1 8.1 9.2 9.2 Level 3 Level 3 0.25 0.25 GOODS-S GOODS-S 34 34 25 25 2.2 2.2 6.2 6.2 6.7 6.7 10.5 10.5 12.7 12.7 14.5 14.5 0.25 0.25 Groth Groth Strip Strip 34 34 25 25 2.2 2.2 6.2 6.2 6.7 6.7 10.5 10.5 12.7 12.7 14.5 14.5 0.25 0.25 Lockman Lockman 34 34 25 25 2.2 2.2 6.2 6.2 6.7 6.7 10.5 10.5 12.7 12.7 14.5 14.5 Level 4 Level 4 2 2 COSMOS COSMOS 110 110 50 50 6.0 6.0 9.8 9.8 10.5 10.5 21.1 21.1 25.5 25.5 29.1 29.1 2 2 XMM-LSS XMM-LSS 110 110 50 50 18 18 9.8 9.8 10.5 10.5 21.1 21.1 25.5 25.5 29.1 29.1 Level 5 Level 5 10 10 Spitzer Spitzer 185 185 200 200 18 18 16.9 16.9 18.0 18.0 23.6 23.6 28.5 28.5 32.5 32.5 Level 6 Level 6 50 50 Spitzer Spitzer - - 150 150 18 18 - - 120 120 61 61 74 74 84 84 Time (hr) : Time (hr) : PACS (659) PACS (659) SPIRE (850) SPIRE (850) Harwit (10) Harwit (10) (Spitzer Depths) (Spitzer Depths) Herschel Extragalactic GT Survey Wedding Herschel Extragalactic GT Survey Wedding Cake Cake Confusion sets in at a flux Confusion sets in at a flux determined by the Beam FWHM determined by the Beam FWHM line (right) line (right) and the 10 bps line (below) and the 10 bps line (below) SPIRE 350 SPIRE 350 PACS 170 PACS 170 PACS 70 PACS 70 (See C) for (See C) for Legenda) Legenda) Integral Counts Integral Counts Rodighiero et al. 2006 Rodighiero et al. 2006 (MNRAS, 371) showed that (MNRAS, 371) showed that using conventional using conventional deconvolution techniques one deconvolution techniques one can use IRAC 3.6 can use IRAC 3.6 m m positions to detect MIPS 24 positions to detect MIPS 24 m sources down to 3 m sources down to 3 ~ 10 ~ 10 bps levels, thus bps levels, thus “extrapolating” by nearly a “extrapolating” by nearly a decade in decade in , as in e.g. , as in e.g. MIPS 24 MIPS 24 m vs SPIRE 250 m vs SPIRE 250 m m MIPS 24 MIPS 24 m m MIPS 70 MIPS 70 m m MIPS 160 MIPS 160 m m SCUBA 850 SCUBA 850 m m z- z- distributi distributi on on MIPS 24 MIPS 24 m m (See C) for (See C) for Legenda) Legenda) … … fitting fitting additional additional observables observables into modeling into modeling picture and picture and applying applying techniques to techniques to other other instruments, instruments, e.g. Akari & e.g. Akari & Planck & SPICA Planck & SPICA & FIRM. & FIRM. Public web page Public web page is also in the is also in the works! works! An Herschel Survey of Surveys An Herschel Survey of Surveys (SOS) (SOS) www.mattiavaccari.net/herschel/sos 3 3 ~ 10 bps ~ 10 bps 3 3 ~ 20 bps ~ 20 bps 10 bps 10 bps 20 bps 20 bps From a From a confusion point confusion point of view, rich of view, rich opportunities opportunities exist to extend exist to extend GT KP mid- & GT KP mid- & large-area large-area planned surveys planned surveys (~ 1 deg (~ 1 deg 2 2 or or larger) to larger) to deeper levels, deeper levels, and and particularly so particularly so on the PACS on the PACS side side Opp. Area Opp. Area Opp. Area Opp. Area What extragalactic OT KP surveys can we ask of What extragalactic OT KP surveys can we ask of Herschel? Herschel?
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Transcript of Extragalactic Confusion Limits in Herschel Key Programs Mattia Vaccari & Alberto Franceschini &...
Extragalactic Confusion LimitsExtragalactic Confusion Limitsin Herschel Key Programsin Herschel Key Programs
Mattia Vaccari & Alberto Franceschini & Giulia Rodighiero & Stefano Berta Mattia Vaccari & Alberto Franceschini & Giulia Rodighiero & Stefano Berta Department of Astronomy - University of PadovaDepartment of Astronomy - University of Padova
Extragalactic Confusion LimitsExtragalactic Confusion Limitsin Herschel Key Programsin Herschel Key Programs
Mattia Vaccari & Alberto Franceschini & Giulia Rodighiero & Stefano Berta Mattia Vaccari & Alberto Franceschini & Giulia Rodighiero & Stefano Berta Department of Astronomy - University of PadovaDepartment of Astronomy - University of Padova
A) SummaryA) Summary ISO, Spitzer & SCUBA counts are used to constrain models of extragalactic populationsISO, Spitzer & SCUBA counts are used to constrain models of extragalactic populations Extragalactic confusion in Herschel bands is estimated using 2 complementary criteriaExtragalactic confusion in Herschel bands is estimated using 2 complementary criteria The two approaches respectively measure cell-to-cell fluctuations due to unresolved The two approaches respectively measure cell-to-cell fluctuations due to unresolved
sources and set a maximum number density for resolved sourcessources and set a maximum number density for resolved sources These two methods provide results which are in good agreement for all Herschel bandsThese two methods provide results which are in good agreement for all Herschel bands Currently envisaged sensitivities for Herschel KP surveys are compared with our Currently envisaged sensitivities for Herschel KP surveys are compared with our
predictions and opportunities for Herschel OT extragalactic KP surveys are outlinedpredictions and opportunities for Herschel OT extragalactic KP surveys are outlined
Mattia VaccariMattia [email protected]
E) “Fluctuations” vs. “Counts” Confusion LimitsE) “Fluctuations” vs. “Counts” Confusion Limits 3 3 “Fluctuations” are very close to “Counts” 10 bps for PACS but nearer to 20 “Fluctuations” are very close to “Counts” 10 bps for PACS but nearer to 20
bps for SPIRE, due to different count slopes at and fainter than 10/20 bps levelsbps for SPIRE, due to different count slopes at and fainter than 10/20 bps levels The availability of multi-The availability of multi- data (e.g. MIPS 24 data (e.g. MIPS 24 m for PACS, PACS & SCUBA2 for m for PACS, PACS & SCUBA2 for
SPIRE, etc) will be invaluable in linking various wavelength regimes and accurately SPIRE, etc) will be invaluable in linking various wavelength regimes and accurately
pin-pointing sources in order to reach down to 10 bps levels in all Herschel bands.pin-pointing sources in order to reach down to 10 bps levels in all Herschel bands.See posters by Franceschini on H-COSMOS and by Dunne & Dunlop on H-SCLS See posters by Franceschini on H-COSMOS and by Dunne & Dunlop on H-SCLS
B) Confusion at Long Wavelengths with HerschelB) Confusion at Long Wavelengths with Herschel Confusion sets a major limit to the sensitivity of long-Confusion sets a major limit to the sensitivity of long- extragalactic surveys extragalactic surveys As IRAS first dramatically showed, the FIR/sub-mm sky is very densely populatedAs IRAS first dramatically showed, the FIR/sub-mm sky is very densely populated ISO & Spitzer & SCUBA confirmed this view providing a wealth of additional dataISO & Spitzer & SCUBA confirmed this view providing a wealth of additional data Great care must be taken in taking stock of current knowledge in order to predict Great care must be taken in taking stock of current knowledge in order to predict
Herschel confusion limits and thus allow a timely planning of GT & OT KP observationsHerschel confusion limits and thus allow a timely planning of GT & OT KP observations
D) Measuring Confusion through “Fluctuations” & “Counts”D) Measuring Confusion through “Fluctuations” & “Counts” ““Fluctuations” measure fluctuations in the background due to unresolved sources Fluctuations” measure fluctuations in the background due to unresolved sources
[Franceschini et al. 1989 (ApJ, 344) ] and set “confusion” at the [Franceschini et al. 1989 (ApJ, 344) ] and set “confusion” at the 3 3 fluctuation level fluctuation level “ “Counts” measure source counts and set “confusion” where a maximum number of Counts” measure source counts and set “confusion” where a maximum number of
sources per beam, or rather a minimum number of beams per source (bps), is reached sources per beam, or rather a minimum number of beams per source (bps), is reached
[Franceschini et al. 2001 (A&A, 378)][Franceschini et al. 2001 (A&A, 378)] Roughly speaking, while “Fluctuations” follow the trend of counts fainter than the Roughly speaking, while “Fluctuations” follow the trend of counts fainter than the
confusion limit, “Counts” follow the trend at brighter fluxes than that. The degree of confusion limit, “Counts” follow the trend at brighter fluxes than that. The degree of
consistency between the two depends on the slope of counts at and near this flux limit.consistency between the two depends on the slope of counts at and near this flux limit.
F) Recommendations for Herschel GT & OT KP PlanningF) Recommendations for Herschel GT & OT KP Planning From a confusion point of view, From a confusion point of view, target sensitivities envisaged in Herschel GT target sensitivities envisaged in Herschel GT
KP surveys appear to be realistic when modeling ISO & Spitzer & SCUBA results.KP surveys appear to be realistic when modeling ISO & Spitzer & SCUBA results. Opportunities exist to go deeper (see posters by Franceschini on H-COSMOS Opportunities exist to go deeper (see posters by Franceschini on H-COSMOS
and by Dunne & Dunlop on H-SCLS) and wider (see posters by De Zotti on SPIRE and by Dunne & Dunlop on H-SCLS) and wider (see posters by De Zotti on SPIRE
LAS and by Serjeant on H-SASSy) over medium- and large-size areas.LAS and by Serjeant on H-SASSy) over medium- and large-size areas. In particular, judging from Spitzer results, reaching the 3 In particular, judging from Spitzer results, reaching the 3 ~ 10 bps levels in all ~ 10 bps levels in all
PACS & SPIRE bands over larger areas than planned in GT KP surveys appears to PACS & SPIRE bands over larger areas than planned in GT KP surveys appears to
be feasible and thus somehow mandatory in order to fulfill Herschel’s potential for be feasible and thus somehow mandatory in order to fulfill Herschel’s potential for
extragalactic surveys. Such deep OT KP surveys should be undertaken over sky extragalactic surveys. Such deep OT KP surveys should be undertaken over sky
areas where deep Spitzer MIPS 24 areas where deep Spitzer MIPS 24 m and/or SCUBA2 coverage is or will soon be m and/or SCUBA2 coverage is or will soon be
available, e.g. within the most popular “Cosmic Windows”.available, e.g. within the most popular “Cosmic Windows”. Survey-like ultra-deep exploratory efforts should be undertaken at a relatively Survey-like ultra-deep exploratory efforts should be undertaken at a relatively
early time during Herschel operations in order to determine actual confusion levels early time during Herschel operations in order to determine actual confusion levels
and test deconvolution techniques in a timely manner, thus ensuring to make the and test deconvolution techniques in a timely manner, thus ensuring to make the
most of Herschel’s 3-year life span.most of Herschel’s 3-year life span.
ChannelChannel PACS1PACS1 PACS2PACS2 PACS3PACS3 SPIRE1SPIRE1 SPIRE2SPIRE2 SPIRE3 SPIRE3
mm 7070 110110 170170 250250 350350 500500
Beam FWHMBeam FWHM 4 .74”4 .74” 6.96”6.96” 10.76”10.76” 17.1”17.1” 24.4”24.4” 34.6”34.6”
3 3 [mJy] [mJy] 0.070470.07047 1.0021.002 7.4847.484 18.1218.12 22.5522.55 20.1920.19
10 bps [mJy]10 bps [mJy] 0.11000.1100 1.2631.263 7.0907.090 14.0014.00 15.2315.23 13.2313.23
20 bps [mJy]20 bps [mJy] 0.30290.3029 2.7462.746 11.8211.82 20.4920.49 21.6521.65 18.3118.31
30 bps [mJy]30 bps [mJy] 0.48870.4887 4.0344.034 15.2315.23 25.4025.40 26.3426.34 21.4921.49
40 bps [mJy]40 bps [mJy] 0.66560.6656 5.1105.110 18.1218.12 29.1829.18 29.9329.93 24.0924.09
50 bps [mJy]50 bps [mJy] 0.83500.8350 6.1076.107 20.4520.45 32.4732.47 33.0533.05 26.1826.18
C) Modelling ISO, Spitzer & SCUBA ObservationsC) Modelling ISO, Spitzer & SCUBA Observations Models by Franceschini et al. 2001 (A&A, 378) were updated to account for intervened Models by Franceschini et al. 2001 (A&A, 378) were updated to account for intervened
reanalyses of ISO 15 reanalyses of ISO 15 m data and results from Spitzer MIPS and SCUBA observationsm data and results from Spitzer MIPS and SCUBA observations Models describe available observables (number counts, z-distributions, L-functions, Models describe available observables (number counts, z-distributions, L-functions,
integrated CIRB levels…), in terms of four populationsintegrated CIRB levels…), in terms of four populations slowly or non-evolving disk galaxies [slowly or non-evolving disk galaxies [blueblue dotted lines] dotted lines] type-1 AGNs evolving as shown by UV and X-ray selected quasars & Seyfertstype-1 AGNs evolving as shown by UV and X-ray selected quasars & Seyferts
[[greengreen long-short dashed lines] long-short dashed lines] moderate-luminosity starbursts with peak emission at z ~ 1 [moderate-luminosity starbursts with peak emission at z ~ 1 [cyancyan dot-dashed lines] dot-dashed lines] ultra-luminous starbursts with peak evolution between z = 2 and z = 4 ultra-luminous starbursts with peak evolution between z = 2 and z = 4 [[redred
long dashed lines]long dashed lines]
NameName AreaArea FieldField PACS PACS TimeTime
SPIRE SPIRE TimeTime 7070 110110 170170 250250 350350 500500
-- deg^2deg^2 -- hrhr hrhr mJymJy mJymJy mJymJy mJymJy mJymJy mJymJy
ClustersClusters -- -- 8080 100100 -- -- -- -- -- --
Level 1Level 1 0.040.04 GOODS-SGOODS-S 230230 1010++3030 1.01.0 1.01.0 1.01.0 3.33.3 4.04.0 4.64.6
Level 2Level 2 0.040.04 GOODS-NGOODS-N 2727 1010 2.02.0 2.82.8 3.03.0 6.76.7 8.18.1 9.29.2
Level 3Level 3 0.250.25 GOODS-SGOODS-S 3434 2525 2.22.2 6.26.2 6.76.7 10.510.5 12.712.7 14.514.5
0.250.25 Groth StripGroth Strip 3434 2525 2.22.2 6.26.2 6.76.7 10.510.5 12.712.7 14.514.5
0.250.25 LockmanLockman 3434 2525 2.22.2 6.26.2 6.76.7 10.510.5 12.712.7 14.514.5
Level 4Level 4 22 COSMOSCOSMOS 110110 5050 6.06.0 9.89.8 10.510.5 21.121.1 25.525.5 29.129.1
22 XMM-LSSXMM-LSS 110110 5050 1818 9.89.8 10.510.5 21.121.1 25.525.5 29.129.1
Level 5Level 5 1010 SpitzerSpitzer 185185 200200 1818 16.916.9 18.018.0 23.623.6 28.528.5 32.532.5
Level 6Level 6 5050 SpitzerSpitzer -- 150150 1818 -- 120120 6161 7474 8484
Time (hr) : Time (hr) : PACS (659)PACS (659) SPIRE (850) SPIRE (850) Harwit (10)Harwit (10) (Spitzer Depths)(Spitzer Depths)
Herschel Extragalactic GT Survey Wedding CakeHerschel Extragalactic GT Survey Wedding Cake
Confusion sets in at a flux determined Confusion sets in at a flux determined
by the Beam FWHM line (right)by the Beam FWHM line (right)
and the 10 bps line (below)and the 10 bps line (below)
SPIRE 350SPIRE 350PACS 170PACS 170PACS 70PACS 70
(See C) for Legenda)(See C) for Legenda)
Integral CountsIntegral Counts
Rodighiero et al. 2006 (MNRAS, 371) Rodighiero et al. 2006 (MNRAS, 371)
showed that using conventional showed that using conventional
deconvolution techniques one can deconvolution techniques one can
use IRAC 3.6 use IRAC 3.6 m positions to detect m positions to detect
MIPS 24 MIPS 24 m sources down to 3 m sources down to 3 ~ ~
10 bps levels, thus “extrapolating” 10 bps levels, thus “extrapolating”
by nearly a decade in by nearly a decade in , as in e.g., as in e.g.
MIPS 24 MIPS 24 m vs SPIRE 250 m vs SPIRE 250 mm
MIPS 24 MIPS 24 mm MIPS 70 MIPS 70 mm MIPS 160 MIPS 160 mm
SCUBA 850 SCUBA 850 mm
z-distributionz-distribution
MIPS 24 MIPS 24 mm
(See C) for Legenda)(See C) for Legenda)
……fitting additional fitting additional
observables into observables into
modeling picture modeling picture
and applying and applying
techniques to other techniques to other
instruments, e.g. instruments, e.g.
Akari & Planck & Akari & Planck &
SPICA & FIRM.SPICA & FIRM.
Public web page is Public web page is
also in the works!also in the works!
An Herschel Survey of Surveys (SOS)An Herschel Survey of Surveys (SOS)www.mattiavaccari.net/herschel/sos
3 3 ~ 10 bps ~ 10 bps
3 3 ~ 20 bps ~ 20 bps 10 bps10 bps
20 bps 20 bps
From a confusion From a confusion
point of view, rich point of view, rich
opportunities exist opportunities exist
to extend GT KP to extend GT KP
mid- & large-area mid- & large-area
planned surveysplanned surveys
(~ 1 deg(~ 1 deg2 2 or larger) or larger)
to deeper levels, to deeper levels,
and particularly so and particularly so
on the PACS sideon the PACS side
Opp. AreaOpp. Area
Opp. Area
Opp. Area
What extragalactic OT KP surveys can we ask of Herschel?What extragalactic OT KP surveys can we ask of Herschel?
