1. Predicting Herschel & SCUBA2 Confusion Measuring “Fluctuations” & “Counts” Mattia Vaccari & Alberto Franceschini & Giulia Rodighiero & Stefano Berta Department of Astronomy - University of Padova A) Summary Confusion in Herschel & SCUBA2 bands is estimated using two complementary criteria Confusion in Herschel & SCUBA2 bands is estimated using two complementary criteria ISO, Spitzer & SCUBA counts are used to constrain models of extragalactic populations ISO, Spitzer & SCUBA counts are used to constrain models of extragalactic populations Based on such models the two approaches respectively measure fluctuations due to unresolved sources and set a maximum number density for resolved sources Based on such models the two approaches respectively measure fluctuations due to unresolved sources and set a maximum number density for resolved sources These two methods provide results which are in good agreement for all bands These two methods provide results which are in good agreement for all bands Recommendations for planning Herschel & SCUBA2 extragalactic surveys are outlined Recommendations for planning Herschel & SCUBA2 extragalactic surveys are outlined Mattia Vaccari mattia@mattiavaccari.net www.mattiavaccari.net E) “Fluctuations” vs. “Counts” Confusion Limits 3  “Fluctuations” are very similar to “Counts” 10 bps for PACS but nearer to 20 bps for SPIRE 3  “Fluctuations” are very similar to “Counts” 10 bps for PACS but nearer to 20 bps for SPIRE This is due to the different slopes of PACS and SPIRE counts at and fainter than their 10 bps levels This is due to the different slopes of PACS and SPIRE counts at and fainter than their 10 bps levels The availability of multi- (notably MIPS 24/70  m and/or PACS) data will be invaluable in accurately pin-pointing SPIRE & SCUBA2 sources in order to reach down to 10 bps fluxes in all Herschel bands The availability of multi- (notably MIPS 24/70  m and/or PACS) data will be invaluable in accurately pin-pointing SPIRE & SCUBA2 sources in order to reach down to 10 bps fluxes in all Herschel bands G) Ongoing Work Fitting additional observables (e.g. redshift distributions) into refined modelling picture Fitting additional observables (e.g. redshift distributions) into refined modelling picture Comparing our estimates with results obtained using other confusion estimators Comparing our estimates with results obtained using other confusion estimators Providing a “consensus“ confusion model suitable for survey planning Providing a “consensus“ confusion model suitable for survey planning Applying techniques to other projects, e.g. Akari & SPICA & FIRM Applying techniques to other projects, e.g. Akari & SPICA & FIRM B) Confusion at Long Wavelengths with Herschel & SCUBA2 Confusion sets a major limit to the sensitivity of long- extragalactic surveys Confusion sets a major limit to the sensitivity of long- extragalactic surveys As IRAS first dramatically showed, the FIR/sub-mm sky is very densely populated As IRAS first dramatically showed, the FIR/sub-mm sky is very densely populated ISO & Spitzer & SCUBA confirmed this view providing a wealth of additional data ISO & 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 Herschel & SCUBA2 confusion limits and thus allow a timely planning of observations Great care must be taken in taking stock of current knowledge in order to predict Herschel & SCUBA2 confusion limits and thus allow a timely planning of observations D) Measuring Confusion with Fluctuations & Counts “Fluctuations” measure fluctuations in the background due to unresolved sources [Franceschini et al. 1989 (ApJ, 344) ] and set “confusion” at the 3  fluctuation level “Fluctuations” measure fluctuations in the background due to unresolved sources [Franceschini et al. 1989 (ApJ, 344) ] and set “confusion” at the 3  fluctuation level “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 [Franceschini et al. 2001 (A&A, 378)] “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 [Franceschini et al. 2001 (A&A, 378)] 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 consistency between the two depends on the slope of counts at and near this flux limit 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 consistency between the two depends on the slope of counts at and near this flux limit F) Recommendations for Herschel & SCUBA2 Survey Planning Target sensitivities envisaged in Herschel & SCUBA2 surveys appear to be realistic from a confusion stand-point when modelling ISO & Spitzer & SCUBA results Target sensitivities envisaged in Herschel & SCUBA2 surveys appear to be realistic from a confusion stand-point when modelling ISO & Spitzer & SCUBA results In particular, reaching the ~10 mJy level in all SPIRE bands appears to be feasible and thus somehow mandatory in order to fulfill Herschel’s potential for extragalactic surveys. Such deep SPIRE surveys should be undertaken over sky areas where deep Spitzer MIPS 24/70  m and/or PACS coverage is or will be available, e.g. within the most popular “Cosmic Windows” In particular, reaching the ~10 mJy level in all SPIRE bands appears to be feasible and thus somehow mandatory in order to fulfill Herschel’s potential for extragalactic surveys. Such deep SPIRE surveys should be undertaken over sky areas where deep Spitzer MIPS 24/70  m and/or PACS coverage is or will be available, e.g. within the most popular “Cosmic Windows” Survey-like exploratory efforts should be undertaken at a relatively early time during Herschel & SCUBA2 operations in order to measure actual confusion levels and thus ensure to make the most of Herschel’s 3-year life span and of SCUBA2’s 2-year & 5-year plans. Survey-like exploratory efforts should be undertaken at a relatively early time during Herschel & SCUBA2 operations in order to measure actual confusion levels and thus ensure to make the most of Herschel’s 3-year life span and of SCUBA2’s 2-year & 5-year plans.ChannelPACS1PACS2PACS3SPIRE1SPIRE2SPIRE3SC2-SSC2-B mmmm70110170250350500450850 Beam FWHM 4.74” 6.96”10.76”17.1”24.4”34.6”7.4”13.7” 3  [mJy] 0.070471.0027.48418.1222.5520.191.9671.383 10 bps [mJy] 0.11001.2637.09014.0015.2313.231.9171.302 20 bps [mJy] 0.30292.74611.8220.4921.6518.313.4262.125 30 bps [mJy] 0.48874.03415.2325.4026.3421.494.6042.755 40 bps [mJy] 0.66565.11018.1229.1829.9324.095.6303.253 50 bps [mJy] 0.83506.10720.4532.4733.0526.186.4673.701 C) Modelling ISO, Spitzer & SCUBA Observations Models by Franceschini et al. 2001 (A&A, 378) were updated to account for intervened reanalyses of ISO 15  m data and results from Spitzer MIPS and SCUBA observations Models by Franceschini et al. 2001 (A&A, 378) were updated to account for intervened reanalyses of ISO 15  m data and results from Spitzer MIPS and SCUBA observations Models describe available observables in terms of four populations Models describe available observables in terms of four populations slowly or non-evolving disk galaxies [blue dotted lines] slowly or non-evolving disk galaxies [blue dotted lines] type-1 AGNs evolving as shown by UV and X-ray selected quasars & Seyferts [green long-short dashed lines] type-1 AGNs evolving as shown by UV and X-ray selected quasars & Seyferts [green long-short dashed lines] moderate-luminosity starbursts with peak emission at z ~ 1 [cyan dot-dashed lines] moderate-luminosity starbursts with peak emission at z ~ 1 [cyan dot-dashed lines] ultra-luminous starbursts with peak evolution between z = 2 and z = 4 [red long dashed lines] ultra-luminous starbursts with peak evolution between z = 2 and z = 4 [red long dashed lines] Confusion sets in at a flux level determined by the Beam FWHM line (left below) and the 10 beams per source line (right below) respectively MIPS 24  m MIPS 70  m (See C) for Legenda) SCUBA2 850 SCUBA2 450 SPIRE 350 PACS 170 PACS 70 NameAreaField PACST ime SPIRE Time 70110170250350500-deg^2-hrhrmJymJymJymJymJymJy Clusters--80100------ Level 1 0.04GOODS-S230 10+30 1.01.01.03.34.04.6 Level 2 0.04GOODS-N27102.02.83.06.78.19.2 Level 3 0.25GOODS-S34252.26.26.710.512.714.5 0.25 Groth Strip 34252.26.26.710.512.714.5 0.25Lockman34252.26.26.710.512.714.5 Level 4 2COSMOS110506.09.810.521.125.529.1 2XMM-LSS11050189.810.521.125.529.1 Level 5 10Spitzer1852001816.918.023.628.532.5 Level 6 50Spitzer-15018-120617484 Time (hr) : PACS (659) SPIRE (850) Harwit (10) (Spitzer Depths) Herschel Extragalactic GT Survey Wedding Cake Differential Counts Integral Counts (See C) for Legenda)