PKS 1830 211 B 0218357 PMN J 0134

PKS 1830 -211 B 0218+357 PMN J 0134 Absorption lines with Françoise Combes November 2019 Chaire Galaxies et Cosmologie

HI intervening absorptions Unbiased view of the HI abundance vs z Galaxy in a group Absorption at z=0. 017 (QSO z=1. 5266) f(CNM) = 0. 27 HI emission and absorption (Gupta et al 2018)

Molecular Absorptions Up to now, only 7 systems: PKS 1413, B 3 1504, B 1740 (self-abs), B 0218, PKS 1830, PMN J 0134: gravit lenses, + G 0248, intervening + local: Cen. A, 3 C 293 (0. 045), 4 C 31. 04 (0. 06), BCG (Hydra, etc. . ) Depend mainly on the background source ~ 30 -100 times more sources with SKA? Combes & Wiklind 1998

Scientific goals 1 Evolution of the HI gas density versus z (Star formation) 2 Detection of molecules at high z much more sensitivity (1 Mo) and complementary to emission 3 evolution of chemical abondances HI, OH, CO, etc a molecular survey possible 4 measure of Hubble constant (gravitational lenses), TCMB 5 variation of constants (a, gp, m= me/mp) Superstrings, Kaluza-Klein, compactified extra-dimensions Predict spatio-temporal variations Uzan (2003), Murphy et al (2003), Chand et al (2006)

ALMA: cold gas in cool core clusters Abell 2597 ALMA CO(2 -1) absorption in front of the AGN synchrotron Red-shifted only Dense clouds fueling the AGN Tremblay et al 2016

CO absorptions HI absorptions 1021 -1023 cm-2 cold (< 40 K) gas present within 30 kpc of the BCG Mainly inflowing when CO Also outflowing in HI N 5044 (David et al 2014) A 2597 Hydra A (Edge et al) 6

Higher redshift absorptions First system towards the BLLac object PKS 1413+135 (Wilkind & Combes 94) after many unfruitful searches towards DLAs Since then, 7 systems are known, but remain rare Three of them are gravitationally lensed objects PKS 1830 -211 and B 0218+357, PMN J 0134 Redshifts range up to z~1 (the QSO at z~2), difficult to find higher redshifts QSO, that are strong enough in the mm (steep spectrum) K-correction is against us! The QSO radio emission decreases with n (up to now, flat-spectrum sources. . ) We should follow the redshift of the radio continuum to cm l

Associated system: PKS 1413+135 z=0. 247 Very narrow absorption < 1 km/s (2 comp) Bl. Lac, very variable, also in radio optically thick, N(H 2) > 1022 cm-2, Av > 30 mag Mc. Hardy et al 94

Intervening: PKS 1830 -211 z=0. 8858 Wiklind & Combes 96 Frye et al 97 2 V-comp, covering each A or B Pd. B (Wiklind & Combes 1998) Slight temporal variability

Measure of Tcmb (z) Low excitation (diffuse gas) Tex ~Tcmb (Wiklind & Combes 98) The case for PKS 1830 -211 Several transitions give the same result (slightly lower, due to a microlens) From UV H 2 lines Srianand et al 2000 Reimers et al 2003 Cui et al 2005

PKS 1830 -211, ALMA OH+, H 2 O +isotopes (Muller et al 2016) Muller et al 2006, low 17 O/18 O, CH+, SH+ Muller et al 2017

Absorption lines with ALMA Absorption in PKS 1830 -211 (z=0. 89), Müller et al 2014, Beelen et al 2015 Constraints on the variation of constants With CH and H 2 O Large diferences between los Da/a < 5. 8 × 10− 7 Variability or Dμ/μ < 1. 2 × 10− 6 Flares of gamma-rays, etc

PMN J 0134 -0931 with ALMA Two lens galaxies merging, z=0. 7645 2 los offset by 5 kpc, 215 km/s D very high in HCO+ HI versus HCO+ Wiklind et al 2018

CO, CN absorption at z=0. 05 in G 0248+430 Two merging galaxies, a tidal tail in front of the remote QSO (z=1. 313) GMRT +NOEMA obs, 17 kpc from G 1 parent Combes et al 2019 Gupta et al 2018

PKS B 1740 -517, ASKAP+ALMA Self-absorbing system at z=0. 44, HI and CO Coincide in the center + outside HI cloud Fueling a young Radio AGN in the center Allison et al 2019

Variation of a B 0218 PKS 1413 Local tests: open symbols QSO absorptions: filled symbols Olive et al (2002) meteorites in solar system

Variation of the mass ratio m=me/mp <Δμ/μ> = (0. 1 ± 0. 5) 10 -6 Radio PKS 1830 B 0218 <Δμ/μ> = (3. 4 ± 2. 7) 10 -6 H 2 Rotation- vibration lines, all dependent on m Electronic lines on a Bagdonaite et al 2013, 14, 15 H 2 in optical Noterdaeme et al 2008, Rahmani et al 2013 17

Why so few radio absorbers? HI Blue: HI absorption Red: cosmic SFD SFRD ~1/Tspin Curran et al (2018, 19) Degeneracy between Tspin Column density, size of the sources Radio spectrum, ionization When T >4000 K 7 in molecules, and 85 in HI-21 cm (z>0. 1)

DLA found in SDSS-BOSS 12 081 with log N(HI) ≥ 20, including 6839 log N(HI) ≥ 20. 3 z>2 Large uncertainty at high NHI Noterdaeme et al 2012

MALS with Meer. KA

MALS with Meer. KAT PI: N. Gupta and R. Srianand (IUCAA) 1655 hrs for the search of HI 21 -cm and OH 18 -cm absorption lines Map the evolution of cold gas in galaxies at 0<z<2 Processing and Archiving infrastructure DB and ARTIP-CUBE in advanced development stage Gupta et al (2017)

Details of the MALS Each pointing will be centered on a >400 m. Jy radio source L-band 1 -deg 2

Number of absorbers versus z Mg. II Intervening HI 21 cm absorbers are now more frequent about a 30% detection rate of optically selected sight lines Mg. II, [Fe. II] (e. g. Dutta et al. 2017) OH absorbers in intervening galaxies are still rare, with an incidence DLA or a number per unit redshift of n. OH = d. NOH=dz = 0. 008, at z ~0. 1 (Gupta et al. 2018)

Comparison other surveys Emission MALS will give a true N(21) and N(OH) at high z, might also detect some emission, OH mega-masers, etc 5 s Gupta et al (2017)

Typical projects with SKA 1 Molecular survey PKS 1413, PKS 1830, Cen. A, etc 7 priority bands, (wide), resolution 1 -4 km/s 2 Search new systems: towards 60 selected radio loud AGNs with mm cont flux > 50 m. Jy Criteria: obscuration, gravitational lensing, suppressed soft X-ray flux Search over the entire redshift range using the technique of frequency scanning.

z-cutoff, Shaver et al (1996) Jackson 2005 Flat-spectrum= beamed BLLac, QSO. . Wall et al (2005) Density of radio quasars (Parkes flat-spectrum, 878 sources) Optical quasars follow the same curve very similar to star formation history

Prospective Number of sources: at low and high z, depends on the N(S) curve, in particular flat spectrum (compact, young AGN) 1 or 2 orders of magnitude Weakened by the non-favorable K-correction in the mm range Very interesting to search 3 mm systems at cm wavelengths, with SKA-1, and also Band 5