Poster'Pop'Session

Crocker, Bicknell, Taylor & CarrettiStar formation-driven Fermi bubbles
Schematic of bubble

Radius as function of timeĖṀ⇠⇠1040 erg s 1
0.08 M y 1

R(t)• Bubble ~108 yrs oldRShock

Rshock/kpc
RShockKinetic luminosity• Reverse shock @ 1-1.5 kpc inexpanding bubble - origin ofmicrowave haze and extended radioemission• Hadronic gamma ray emission fromshell inside bubble1

Statistical Challenges in Fitting Stellar Orbits
Around the BH at the Galactic Center.
Gregory Martinez1, Kelly Kosmo1, Aurelien Hees1, Joseph Ahn1 and Andrea Ghez1
1
University of California, Los Angeles
Raw pixel
CountsGC Group/Keck pipeline

Background
Background
Substraction
Substraction(ideally)(ideally)

GradStudent

PSF
PSF
Extraction
Extraction

SourceSourceDetection
Detection

We have over 20 years of stellar databut our measurements are limited by
the precision of our reference frame.
Currently We estimate our reference
errors by Jack Knifing. But, global
likelihood analysis is on the way!

Reference
Reference
Frame
Frame
Alignment
Alignment

Stellar
StellarOrbitalOrbitalAnalysisAnalysis

Stellar orbital analysis presentsinteresting statistical challenges suchas exploring large dimension
parameter spaces and testing forstatistical consistency.
My poster details coverage tests of
BH parameter's confidence intervels
assuming various priors, include our“observational-based” priors.

Herschel(far+IR(&(submm(spectroscopy(of(Sgr(A*(and(the(CND!!
Javier(R.(Goicoechea1,*((Mireya(Etxaluze1,2((José(Cernicharo1((Jerome(Pety3((and(collaborators(1Grupo de Astrofísica Molecular, ICMM-CSIC, Madrid, Spain.

2RAL, Oxford, UK.

3IRAM-Grenoble, France!(DistribuNon(of(ionized,(neutral(atomic,(warm(molecular(gas(with(Herschel/PACS((a)b)!(Line(proﬁles(with(Herschel/HIFI(c)!(Working(on(our(ALMA(images…((7’’!

-0.300 -0.200 -0.100 0.000 0.100 0.200

Galactic latitude [deg]PACS/HERSCHELLABOCA/APEX
HCN /Mopra

The Bubble in the
Galactic Center!

M. A. Requena Torres; A.
Noriega-Crespo; A. Harris

The Brick

Sgr B2!!

0.800

Thermal Filaments

Sgr C

Sgr A!!

!!

0.600

!!

0.400

0.200

!!

0.000

!!

359.800!!

359.600

Galactic longitude [deg]Work in progress
1

1.3

1.7

2

2.4

2.7

3

3.4!!

359.400

3.7

We try to compare the neutral molecular gas,ionized molecular gas and dust emission inthe bubble of the Galactic Center. We use as
starting point the data observed with Herschel.

SPLASH OH masers in the Galactic Centre region

TheOHmas
erdi
str
i
buti
oni
nt
heGal
act
icCentr
eregi
on.
1

Star formation rates on global and cloudscales within the Galactic CentreA.T.$Barnes,$S.N.$Longmore,$C.$Battersby,$J.$Bally,$J.$M.$D.$KruijssenDaisuke Sakai (Univ. of Tokyo)
VLBI astrometry toward Sgr D HII region with VERA
Astrometric results for water maser in Sgr D(b)

0-6-8Offset (mas)-2Offset (mas)Decl. offset (mas)(a)-4-6-8-10-10-2-4

R.A. offset (mas)

-6

2010

2011

Year1
0.8
0.6
0.4
0.2
0-0.2
-0.4
-0.6
-0.8
-1
-1.2
-1.4
-1.6
-1.8
-2
2010

(c)

2011

YearParallax distance is 2.36(-0.39/+0.58) kpc

Future plans

which suggests this source is located at Scutum arm

One of reasons for the diﬃculty of astrometry in GC
is weakness of position reference QSO
By using Sgr B2 water maser as a reference,
we can measure absolute positions of weaker maser
sources than before. (10 Jy to 2-3 Jy)

Preliminary result in my poster

SgrB2

Constraining the Variability
and Binary Fractionof Young Stars in the Galactic Center

Abhimat Gautam
UCLA Galactic Center Group

Keck Adaptive Optics photometric data set over 12 years
Photometric analysis can identify stellar variability and binarity
Variability and binarity helpful for understanding origin of young stars

Initial constraints on the variability of binary fraction of young stars
1.050
0.8

Binary Fraction

Number of Stars

4030

0.60.4200.2

1000.0051015202

red2530

35012345678
Number of Binary Stars Detected

91051040
1198log(p)764Statistical Study of High-Velocity Compact Clouds
Based on the Complete CO Imagings of theCentral Molecular Zone
Sekito Tokuyama, et al. Keio University
We performed a complete CO J=1–0 imaging of the CMZ and developed
an automated procedure to identify High-Velocity Compact Clouds (HVCCs).
CO J=1‒013CO J=1‒0CO J=3‒2C18O J=1‒0Galactic Latitude [degrees]

120.2

120-0.2

10

Galactic Longitude [degrees]

b=0.0215

VLSR = 125 km s 1HVCC
CO 0.02–0.02

We identified 116 HVCCs
and performed statistical study.

Time Evolution of the Giant Molecular Cloud Mass Functions across Galactic Disks

Masato I.N. Kobayashi (Nagoya U)

1) Inutsuka+ 20153) Successfully reproduce observed
variation of GMC mass functions.
(MINK+ 2016 in prep)

Cloud-Cloud Collisions (CCCs)Fukui+ 2014
Nakamura+ 2012
Torii+2015
etclog(ncl [/kpc3/M ])4

Tf ,fid = 10.0 [Myr]Td = 14.0 [Myr]20Time [Myr]-220406080120160200-4-6-8234567log(GMC Mass [M ])2) Formulate coagulation equationof GMC Mass Function4) Observations may put unique constraints

on GMC formation/dispersal timescales
by observing the mass function slope.
Steady State SolutionBACKGROUND INFRARED SOURCES FOR STUDYING
INTERSTELLAR GAS IN THE CENTRAL MOLECULAR ZONETom Geballe (Gemini) et al.
Motivation:

Spectroscopy*of*H3+ has*revealed*long*columns*of*diffuse,/warm,/expanding/gas
on*sightlines*toward*the*center*of*the*CMZ.
Is#this#gas#present#throughout# the#CMZ?
Need*high?resolution*IR*abs.*spectroscopy*of*H3+ on*widely*spaced*sightlines.*! Need*to*find*bright/IR/sources/with/“featureless”/spectra/elsewhere*in*the*CMZ.*
Problem:*vast*majority*of*bright*IR*stars*in*
the*GC*are*red*giants.
red*giant*spectrum

Project:
Use*2MASS*and*Spitzer*(GLIMPSE)*catalogues*to*identify*candidate*dust?
embedded*objects*in*the*
CMZ.*Obtain*quick*low?res.*
K?band*spectroscopy*(mostly*in*Gemini*poor*weather*time)*to*weed*out*RGs.*

Results: >500*objects*surveyed.
Mostly*(cool)*RGs,*but*also*a*menagerie*of*other*useful*and*interesting*objects (pure*dust*
continua,*heavily*veiled*RGs,*hot*stars).
To*see*more*examples*and*learn*what*we*are*finding*by*using*them*visit*Poster*Board*7!

012

3

4

5

6CND

40

60

80

–0.02 –0.04 –0.06 –0.08 –0.10 –150

2535 s
40 s
45 s
E17 h
45 m50 s

N–0.10 –0.08 –0.06 –0.04 –0.02–100+20 km/s cloud

100–100

Galactic Longitude [deg]4ring

20+20 km s–1 cloud

C1

VLSR = –40 ~ +10 km s–1

0+50 km s–1 cloud

NLEb"V$diagram

CS 2–1–02ʼ

100C–01ʼ

50/G 5D

9°00
ʼ2-pc

–0.10 –0.08 –0.06 –0.04 –0.02/+
5 5 ()

D–2CNDring

5CC5   C1

2-pc

4
G

5 5

5D +NLE0

5 25

G 5D G
G2-pc ring–50,5 5G

Galactic Latitude [deg]5Galactic Latitude [deg]5LSR Velocity [km s–1]

05 pc

D5DC5D–50050

LSR Velocity [km s ]–1100–0.02 –0.04 –0.06 –0.08 –0.10

Galactic Longitude [deg]K DK/+G 5/+

55CG,.