The WEAVE-QSO Survey Mat Pieri - and the WEAVE Collaboration - Projects at LAM
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IPhU CLASS meeting 23rd Sept 2021 The WEAVE-QSO Survey Mat Pieri and the WEAVE Collaboration
WQ Meeting 8th Sept 2021 Quasar Spectra and Lyman-α Forest Quasar Intergalactic medium Line-of-sight probe of the IG ⇢ Gas with 1 . . 10 ⇢¯ traces dark matter on large scales Largely photoionized ⌧HI / ⇢1.7 H an f = CF = Ce ⌧HI Departures from thi UV background modulatio Strong line Small scale physic credit: Andrew Pontzen Metal absorption The Intergalactic medium dominates the universe by mass and volume s d s s n M
IPhU CLASS 23rd Sept 2021 WEAVE-QSO: The Big Questions Q1: How does dark energy emerge to dominate the out ow universe? in ow expansion ~200 kpc ~150 Circumgalactic Medium (CGM) Mpc Q2: How do quasars galaxies form Q3: What is from IGM? the nature of Lines of sight dark matter? Q4: How does (re)ionization occur? Addressed by WEAVE-QSO through high spatial and spectral resolution fl fl
IPhU CLASS 23rd Sept 2021 WEAVE in a Nutshell New spectrographic survey facility for the 4.2m William Herschel Telescop Fide- eld multi-object spectrograph with integral eld unit WEAVE survey 70% of WHT tim 1st light in Q1 202 Over 400 members over 11 countrie WEAVE-QSO around 5 Open model membership based mostly on nation But institutional and individual buy-in is possibl More members and partners welcome not to scale not to scale WEAVE Consortium Members | June 2016 | Shoko Jin fi s e fi s 2 0 e e s
IPhU CLASS 23rd Sept 2021 Multi-Object Spectroscopy Mode MOS: WEAVE-QSO’s main survey mode in dark time WEAVE collaboration in prep Low resolution: R=4000-7500 High resolution: R=16000-23000
IPhU CLASS 23rd Sept 2021 Integral Field Unit Modes LIFU and mIFU: recent WEAVE-QSO addition as a ller program WEAVE collaboration in prep fi
IPhU CLASS 23rd Sept 2021 The WEAVE Primary Science Surveys The WEAVE Survey consists of 8 primary science surveys 3 Galactic surveys Galactic Archaeology (STL:V. Hill, OCA SCIP (Stellar, Circumstellar, and Interstellar Physics – STL: J. Drew, Herts White Dwarfs (STL: B. Gänsicke, Warwick and 5 Extragalactic surveys WEAVE-Clusters (STL: J. A. Aguerri, IAC WEAVE-Apertif (STL: J. Falcón Barroso, IAC StePS (Stellar Population Survey at intermediate redshifts – STL: A. Iovino, Milano WEAVE-LOFAR (STL: D. Smith, Herts WEAVE-QSO (STL: M. Pieri, LAM) ) : : ) ) ) ) ) : )
IPhU CLASS 23rd Sept 2021 WEAVE-QSO Transforms the Landscape High spectral resolution (R=6000 or 20000 High delity recovery of galaxies in absorption (particularly metals Measure smaller line-of-sight structure for thermal history (reionisation), sum of neutrino masses and exotic dark matte High spatial resolution from dense sample of quasar Measure BAO in large 3D structur Map the cosmic web using IGM tomograph AGN environments, pressure support, detect galaxies in absorption, CW emission fi r ) e y ) s
IPhU CLASS 23rd Sept 2021 WEAVE-QSO Survey Plan Sketch “High resolution” massive IGM surve Spectral res LR: 3xBOSS (2xDESI), or HR: 12xBOSS (9XDESI Spatial res - quasar number density: 4-5 x BOSS ~2 x DES + LIFU (quasars multiplexes) and mIFU (galaxies in absorption MOS survey elds shared with Galactic Archeology and LOFA Goal: 400,000 quasar spectra with z>2.1 and mr
IPhU CLASS 23rd Sept 2021 J-PAS and WEAVE-QSO J-PAS imaging with 54 narrow lters ideal for quasar identi cation Memorandum of understanding signed between the two surveys for Sharing targets and spectr 6000 WEAVE bre hours awarded to J-PA Joint science (e.g. forest and image cross-correlation potential) Bonoli+ 2021 fi fi a fi S
WQ Meeting 8th Sept 2021 Projected BAO constraints WEAVE-QSO BAO ~6000 deg2 J-PAS targeted footprin DESI: more Lyα quasars but lower densit ∝ 1/Density and ∝1/√Are WEAVE-QSO bre hour constrained - choose between z2.4 25% smaller errors at z>2.4 12% smaller errors at z
IPhU CLASS 23rd Sept 2021 IGM Tomography in WEAVE-QSO The next frontier of galaxy formation and cosmology: mapping at z> Large-scales allow novel cosmology (e.g. void counts, critical points etc Small-scales allow big picture on galaxy formation at cosmic noo See Katarina’s talk 0.5 or igin a l field m r
IPhU CLASS 23rd Sept 2021 WEAVE-QSO as a Tomography Pilot DESI also (plan under discussion) Note: I am a new coordinator of MOSIAC SWG2
IPhU CLASS 23rd Sept 2021 Absorber Science in WEAVE-QSO A zoom of SBLA composite Flux Recovery of DLAs and LL New sample: Strong-blended Lya Common: Wavelength Rare: SiIV SiII Public absorber catalogue with high legacy valu Circumgalactic model Galaxy formation at SFR peak: Combination with cosmic web and galaxy surveys Log N Ionization IGM standard e S
IPhU CLASS 23rd Sept 2021 Line-of-sight Forest Power Spectrum WEAVE resolution for small-scale structure suppressio Reionization/thermal history Neutrino masse Cold DM, Warm DM, Fuzzy DM Peeples+2010 s n
IPhU CLASS 23rd Sept 2021 Whats new? IFU as ller program Moderate seeing and grey time: MiniIF Galaxy and quasar environments in emissio Comparison to MUSE (Fossati et al 2021) 0.5 or igin a l field m r
IPhU CLASS 23rd Sept 2021 Whats new? Reviewing Survey Plan WEAVE delays with respect to DES J-PAS delays to give targets to WEAVE-QS CW given greater priority More large-scale multiplet BAO get boost by going fainter to mr
IPhU CLASS 23rd Sept 2021 Summary WEAVE will span the full range of astrophysics on stellar scales to the largest structures measure From our region of the Milky Way to beyond reionizatio WEAVE-QSO is diverse From small-scales (in the CGM) to the CW laments to the largest scale Measuring galaxy formation and early dark energ Entering an exciting and busy period science pay off is coming soon! s d fi y n
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