1. ‘The chase for Minihalos ‘ (or whatever the title I sent in was) or “From High Velocity Clouds to High Velocity Clouds, to High Velocity Clouds, by the way of TF” by the way of TF” Riccardo Giovanelli Riccardo Giovanelli Cornell University Cornell University Green Bank, April 2012

2. Credit: Virgo collaboration (MPIfAp) Numerical simulations predict the existence of lots of low mass halos: Do they exist in the expected numbers? Are baryons blown away by the first generation of stars?Are baryons blown away by the first generation of stars? Is gas accretion & cooling impeded by UV heating in low M halos?Is gas accretion & cooling impeded by UV heating in low M halos? Are baryons retained but unable to make stars?Are baryons retained but unable to make stars? Is that more likely in cosmic voids?Is that more likely in cosmic voids? The Missing Satellite Problem Klypin et al 1999 Tikhonov & Klypin (2009) claim observations fall short by factor > 10

3. HVCs: an Intergalactic Population? Blitz et al (1999):” HVCs are large clouds, with typical diameters of 25 kpc, containing 3x10 7 solar of neutral gas and 3x10 8 solar of dark matter, falling towards [the barycenter of] the Local Group; altogether the HVCs contain 10 10 solar of neutral gas.” Braun & Burton (1999): The “undisturbed” minihalos appear as Compact HVCs, which have typical sizes of 0.5 deg and FWHM linewidts 20-40 km/s Problems: 1. If HVCs (or CHVCs) are bona fide LG members, they should also exist in galaxy groups other than the LG: NOT SEEN (see DJ) 2. Sternberg et al (2002) show that, in order to fit DM halo models to the CHVCs, their HI fluxes and angular sizes constrain them to be no farther than 150 kpc, else they famously violate the  CDM mass-concentration relation: CHVCs ARE TOO LARGE

4. -Hoeft et al. (2006) simulated the SF processes in voids, using code that included radiative processes, SN feedback and an external, photoionizing Hardt & Madau (1996) UV background, with a resolution that allows monitoring evolution of DM halos of mass as low as 2.3x10 8 Msun. - Small halos DO NOT retain their share of baryons  - Note dependence on simulation resolution Characteristic halo Mass M c : that which retains 50% of its baryons Simulations with Gastrophysics

5. Sternberg, McKee & Wolfire (2002) have investigated the gastrophysics of minihalos: the remaining baryons in a low mass halo are capable of developing a small WARM NEUTRAL phase (WNM), possibly detectable through its HI emission. … ‘though HI mass only a fraction of baryon mass Do we have any chance to ever observe these guys? 10 9 Msun halo  < 10 7 Msun baryons

6. Sternberg, McKee & Wolfire 2002 A plausible model for a baryon-poor minihalo: Mass of the Warm, ionized gas (WIM) Virial Halo Mass ALL PLOTS Contours of HI (WNM) radius (kpc) HI column density HI Mass ALFALFA can detect this kind of beast out to 2-3 Mpc

7. … so let’s look nearby

8. Substructure in the Local Group Giant spirals dSph (+dEll) dIrr dIrr/dSph Gas-rich dwarfs live in the periphery of the LG

9. Note

10. … so let’s look nearby for something that looks like: Angular diameter : < 10’ Linewidths: 15-30 km/s Peak flux: tens of mJy

11. cz=264 km/s W50=24 km/s M HI =3.1x10 5 D 2 M sun

12. Credit: T. Osterloo, Spineto 2007 HI mass = 3x10 5 Msun HIMass/L_V = 5 M_dyn=8x10 6 Msun … and still forming stars… [80% of visible baryons in HI]

13. HVCs in footprint of ALFALFA, North Galactic Cap  = 1620 sq deg  = 1620 sq deg N=71 positive HVCs  V LSR >130 km/s N=44 negative HVCs  V LSR <-100 km/s LG galaxies

14. HVCs in footprint of ALFALFA, North Galactic Cap  = 1620 sq deg LG galaxies within D=2.6 Mpc (away from center of LG) V_LSR [km/s]

15. 22 minihalo candidates RG+ (2010) Distances are not known Note: Leo T would not be detectable in either SDSS or DSS if d=1 Mpc Betsey Adams preparing a broader catalog of minihalo candidates

16. ALFALFA Minihalo Candidates at D=1 Mpc Mean HI Mass 3x10 5 solar Mean HI Diameter 0.7 kpc Mean avged HI column density 10 19.1 cm -2 Mean avged HI density 0.006 cm -3 Mean total mass within R HI 3x10 7 solar Sternberg et al (2002) Minihalo Template @ P=10 cm -3 K HI Mass 3x10 5 solar HI Diameter 0.7 kpc Peak HI column density 10 19.6 cm -2 WIM Mass 6x10 6 solar Total mass within R vir 3x10 8 solar At the distance of nearby groups of galaxies, the ALFALFA minihalo candidates would have been below the sensitivity limit of extant HI surveys.

17. We have found a subset of the HVC phenomenon that appears to be compatible with the minihalo hypothesis. Other interpretations are possible, we have not proved that the candidates are LG minihalos, but that is a tantalizing possibility. We need to detect similar features in nearby galaxy groups. That will require - significant increase in telescope survey speed and/or - deep optical images searching for optical counterparts

18. WIYN image, credit: J. Salzer & K. Rhode

19. Looking for P1 analogs beyong the LG In the absence of a stellar component, it is impossible to determine distances to HI minihalo candidates in the LG  Solution: look in nearby groups (D ~3-5 Mpc) for which redshift can imply group membership ( “a’ la DJ”)  Need: coverage of several 100 sqd and 10X ALFALFA sensitivity “AO40” – 40 beam phased array feed Cryogenically cooled, proposed by Cornell in 2007 and currently being prototyped by Cornell/BYU for use at AO With some luck, we could begin such a survey in 2014. 19-beam PAF (Cornell/BYU) prototype for “AO40”

20. To obtains a template TF relation, use a basket of clusters... … + calibrators: over the volume sampled by the template: H_o = 69+/-6 (km/s)/Mpc averaged over a volume of cz = 9500 km/s radius (Giovanelli+ 1996). …and confirm the kinematic nature of the Dipole of the Peculiar Velocity Field … and convergence to the CMB dipole is confirmed by the LG motion w.r.t. a set of 79 clusters out to cz ~ 20,000 km/s