The jet and the disk of the HH 212 low-mass protostar imaged
by ALMA: SO and SO2 emission
L. Podio, C. Codella, F. Gueth, S. Cabrit, R. Bachiller, A. Gusdorf, C.-F.
Lee, B. Lefloch, S. Leurini, B. Nisini, and M. Tafalla• ALMA (Cycle 0),345 GHz band
• SO, SO2 , C17O, CO,SiO)• Kinematics for jetand outflow from aClass 0 protostar• SO and SO2
compared to CO,
SiO…

• SO and SO2 are effective tracers of the molecular jet in theinner few hundreds AU from the protostar.
• The SO abundance in the disk is 3 − 4 orders of magnitudelarger than in evolved protoplanetary disks. This may be due
to an SO enhancement in the accretion shock at theenvelope-disk interface or in spiral shocks if the disk is partly
gravitationally unstable.

A universal, turbulence-regulated star formation law: fromMilky Way clouds to highredshift disk and starburst galaxies
Diane M. Salim, Christoph Federrath and Lisa J. Kewley• previous study: In K-S law, the observed scatter in SFR (for a givengas or gas/tff) can be primarily attributed to the variation in thesonic Mach number of the turbulence in the star-forming clouds.
• Problem in previous work by Krumholz et al. (2012)• Refinement was achieved by expressing the K-S law with gas/tff• The model uses averaged surface density and average freefall time. The
wide distribution of densities withint the ISM/clouds is not taken intoaccount.
→ incorporate the probability density function (PDF) in this study, and multifreefall concept (tff depends on the density)=New SF lawX• Observations: 11 galactic, SMC• Better fit by a factor of 3—4 (goodness-of-fit R2 = 0.97)

Mach number can bepredicted forextragalactic sources
using the new SF law.

V409 Tau As Another AA Tau: Photometric Observations ofStellar Occultations by the Circumstellar Disk
Joseph E. Rodriguez, Joshua Pepper, Keivan G. Stassun, Robert J.
Siverd, Phillip Cargile, David A. Weintraub, Thomas G. Beatty, B. Scott
Gaudi, Eric E. Mamajek, Nicole Sanchez• Optical photometric monitoring ofAA Tau and V409 Tau• good use of data/instruments for
exoplanetary transits• AA Tau & V409 Tau• Showing short-timescale variation(day—week)• AA Tau• Deep, dimming event in 2011,
lasting at least until winter in 2013
• Occultation by dense part of the disk
at >8 AU (M* = 0.85 M).
[Confirmation of Bouvier et al. (2013)]• i~71 deg, a=7.7 AU → h=7.7 AU for
the occulterHot dust revealed during the dimming of the T Tauri star RW Aur A
Victor Shenavrin, Peter Petrov and Konstantin Grankin• IR photometric monitoring of RW AurAB system• RW Aur AB•  = 1.4”, 1.4 M + 0.8 M

• RW Aur B• WTTS (weak accretion)•  =0.12”, M3<0.045 M

• Variability in previous study

Dai et al. (2015)• Long-lasting dimming event in 2010
Duration of several month, depth~2 mag in
opticalObscuration by tidally-disrupted disk?

• Dimming event in 2014, faded by ~3 mag
Cabrit et al. (2006)• IR photometry (1—5 micron) with 125cm telescope (A and B are
not resolved. Most IR emission comes from A.)• IR slope is different between the brighter and fainter phases. Whenthe star fades in optical, additional ~1000 K body is required→ hot dust near the dust sublimation temp (~0.1-0.2 AU)? UXOrilike variability? (should not be the occultation by the distant arm)
• Disk inclination=30—45 deg. Accretion rate remained as usual.
→ Dust in the wind? (the wind was enhanced during the event)Dense Clumps and Candidates for Molecular Outflows in W40
Tomomi Shimoikura, Kazuhito Dobashi, Fumitaka Nakamura,
Chihomi Hara, Tomohiro Tanaka, Yoshito Shimajiri, Kouji Sugitani andRyouhei Kawabe