science overview & publications · • cycle 1: jan 2013-may 2014 (1131 proposals, 800h): –...

1 ANASAC Meeting – May 20, 2015

Al Wootten

Science Overview & Publications


Assess scientific outcomes and impact from Cycles 0, 1 & 2. What are the challenges for NA? ALMAhas produced more than 220 refereed publications •  Wordle from all abstracts


ALMA Observations Thus Far

•  Science Verification: 16 Datasets so far •  Cycle 0: Sep 2011-Dec 2012 (990 proposals, 500h):

–  16 12-m antennas –  Receiver Bands: 3, 6, 7 and 9 –  Highest angular resolution: 0.2”, longest baseline ~ 400 m –  All data delivered

•  Cycle 1: Jan 2013-May 2014 (1131 proposals, 800h): –  32 12-m antennas and ACA (9 7-m antennas, 2 Total Power antennas) –  Receiver Bands: 3, 6, 7 and 9 –  Highest resolution 0.08”, longest baseline ~ 1 km –  Data delivery in progress –  Carry over to Cycle 2 ~ 460 hours


ALMA Observations Thus Far

•  Cycle 2 - June 2014 ! October 2015 "  1384 proposals received for a total of 2000 hours "  353 A & B rated proposals / 159 C rated proposals (fillers)

–  34 12-m antennas and ACA (10 7-m antennas, 2 Total Power antennas; this is the target, which is almost surpassed every night!

–  Receiver Bands: 3, 4, 6, 7, 8 and 9 –  Longest baseline 1.5 km Note: There is a carry-over from Cycle 1 of ~ 460 hours

Cycle 3 - October 2015 ! October 2016 –  1582 proposals received seeking 9037 hours from 2100 hours available –  36 12-m antennas and ACA (9 7-m antennas, 2 Total Power antennas –  Receiver Bands: 3, 4, 6, 7, 8, 9 and 10 –  Longest baseline (10 km, 5km, 2km [(Bands 3,4 and 6)(b7), B8,9,10)] –  In processing


ALMA Science Output

•  Refereed Papers – Data collected May 4, 2015 •  High impact in all subject areas (Highest in Cosmology, Star & Planet Formation) •  Compared with Oct. 31, 2013 ASAC Report •  From ALMA Archive database

–  220 (65) Published –  164 (36) Cycle 0 data –  20 (0) Cycle 1 data (incl. DDT) –  50 (29) Science & Verification data –  16 (7) in Nature/Science

•  Maintaining at ~7-8%

Planet Forma,on Solar System

Cosmology

ISM

Stars and Stellar Envelopes


Forma,on of the 1st Galaxies•  ALMA observation of distant Lyα

entities: –  Deep non-detections in

250GHz continuum and [CII] –  “Himiko” and IOK-1 have very

low dust content and atomic carbon (e.g. metal poor system) – [CII] may not be the best tracer for 1st galaxies

•  Possibly witnessing an assembly of ‘first galaxy’

[CII] [CII]

4 Ouchi et al.

Fig. 3.— Color composite image of Himiko. Blue and green rep-resent HST/WFC3 continua of J125 and H160, respectively. Redindicates Lyα emission resolved with sub-arcsec seeing Subaru ob-servations. The Lyα emission image comprises the Subaru NB921narrowband data with a subtraction of the continuum estimatedfrom the seeing-matched HST/WFC3 data. The three continuumclumps are labeled A, B and C.

of Himiko at 9233A (Ouchi et al. 2009a) with a systemthroughput of 40%, close to the peak throughput of thisfilter (∼ 45%). Thus, the F098M image is ideal for formapping the distribution of Lyα emitting gas.Our observations were conducted in 2010 September

9, 12, 15-16, 18, and 26 with an ORIENT of 275 de-grees. Some observations were partially lost becauseHST went into ‘safe mode’ on 2010 September 9, 22:30during the execution of one visit. The total integra-tion times for usable imaging data are 15670.5, 13245.5,18064.6 seconds for F098M , J125, andH160, respectively.The various WFC3 images were reduced with WFC3and MULTIDRIZZLE packages on PyRAF. To optimizeour analyses, in the multidrizzle processing we chose afinal pixfrac= 0.5 and pixel scale of 0′′.05132. We de-graded images of F098M and J125 to match the PSFsof these images with the one of H160that has the largestsize among the HST images. We ensured the final WFC3images have a matched PSF size of 0′′.19 FWHM.Figure 3 presents a color composite HST UV-

continuum image of Himiko, together with a large ion-ized Lyα cloud identified by the Subaru observations(Ouchi et al. 2009a). This image reveals that the systemcomprises 3 bright clumps of starlight surrounded by avast Lyα nebula ! 17 kpc across. We denote the threeclumps as A, B, and C. Figure 4 shows the HST, Sub-aru, and Spitzer images separately. The F098M imagein Figure 4 detects only marginal extended Lyα emission,because of the shallower surface brightness limit of the2.4m HST compared to the 8m Subaru telescope. Never-theless, we have found a possible bright extended compo-nent at position D in Figure 4. We perform 0′′.4-diameteraperture photometry for the clumps A-C and location Das well as 2′′-diameter aperture photometry which weadopt as the total magnitude of the system. Tables 2and 3 summarize the photometric properties. It shouldbe noted that Himiko is not only identified as an LAE,but also would be regarded as a LBG or ‘dropout’ galaxy.

Fig. 4.— HST, Subaru, and Spitzer images of Himiko; northis up and east is to the left. Each panel presents 5′′ × 5′′ im-ages at F098M , J125, and H160 bands from HST/WFC3, 3.6µmand 4.5µm bands from Spitzer SEDS. The Lyα image is a SubaruNB921 image continuum subtracted using J125 and includes in-tensity contours. The Subaru image has a PSF size of 0”.8. Thered-solid circles indicate the positions of 0′′.4-diameter aperturesfor Clumps A, B, C, and D photometry in the HST images (seeSection 2.2 for details), while the red-dashed circles denote 2′′-diameter apertures used for the defining the total magnitudes.

Using the optical photometry of Ouchi et al. (2009a) (seealso Table 3), we find no blue continuum fluxes for the fil-ters from B through i′ to the relevant detection limits of28−29 mag. The very red color of i′−z′ > 2.1 meets typ-ical dropout selection criteria (e.g. Bouwens et al. 2011).Because the z′-band photometry includes the Lyα emis-sion line and a Lyα-continuum break, we can also esti-mate the continuum-break color using our HST photom-etry of J125 and H160 and the optical i-band photometry.Assuming the continuum spectrum is flat (fν =const.),we obtain a continuum break color i′ − J125 > 3.0 ori′ − H160 > 3.0, further supporting that Himiko as aLBG. Importantly, these classifications apply also to theclumps A-C ruling out that some could be foregroundsources.The UV continuum magnitudes of clumps A-C range

from 26.4 to 27.0 magnitudes in J125 and H160. Eachclump has a UV luminosity corresponding to the char-acteristic luminosity L∗ of a z ∼ 7 galaxy, m=26.8mag (Ouchi et al. 2009b; Bouwens et al. 2011)). More-over, the variation in luminosity across the components issmall; there is no single dominant point source in this sys-tem, confirming earlier deductions that the system doesnot contain an active nucleus.The F098M image shows that Lyα emission is not uni-

formly distributed across the 3 clumps. Clump A showsintense Lyα emission with a rest-frame equivalent width(EW0) of 68

+14−13A placing it in the category of a Lyman

alpha Emitter (LAE), whereas clumps B and C are haveemission more typical of Lyman break galaxies (LBGs)with a rest-frame Lyα equivalent width (EW0) less than

Top: Himiko Ouchi et al. (2013), Bottom: IOK-1 Iye, Ota, Kashikawa et al (2006), Ota and Walter et al. (2014)

AAS225


Gravitational Lensing Galaxy Abell 1689

•  A1689-‐zD1, a dusty, normal galaxy in the epoch of re-‐ioniza,on at z=7.5±0.2 (spectroscopic detec,on of the Lyα Break – Xshooter with VLT)

•  Detected with ALMA at ~230 GHz Sν = 0.61± 0.12 mJy

•  Highly evolved galaxy: large stellar mass (1.7x109 MO), dust enriched (4x107 MO), and gas-‐to-‐dust ra,o close to MW.

•  SFR~12 MO yr-‐1

Watson et al. Nature (2015)


SDP.81 at z = 3.04


ALMA Partnership, Vlahakis et al. 2015


The Long Baseline Campaign: SDP.81 at z=3.04

ALMA Partnership, Vlahakis et al. 2015 0.01”= 400 pc at z=3


Revealing the Complex Nature of SDP.81

Dye et al. 2015 (see also Rybak et al.)


Long Baseline Campaign: HL Tau


Long Baseline Campaign: HLTau

•  Young Star ~1 Million Years •  One of the nearest star forming

regions to Earth (~450 light yr) •  Resolution is 5 AU •  Gaps almost certainly reflect young

planets •  Comparison to Hubble shows

ALMA’s power! •  Presence of several planets at such

a young age is “disturbing” to planet formation theories

ALMA Partnership, Brogan et al. 2015


Long Baseline Campaign: Juno

ALMA Partnership, Hunter et al. 2015

Band 6 -‐ Frequency = 233 GHz; Five consecu,ve execu,ons over 4.4 hours

Beamsize ~ 0.04”x0.03” (~60x45 km)


ALMA Science Output Refereed Papers: Data Collected 4 May 2015 •  Compared with 2014, 2013 ANASAC F2F; All Executives, all cycles •  All ALMA papers tracked by NRAO (and ESO) libraries

–  220, (118, 68) refereed papers with >2500* (1091, 143) citations –  h-index: 31 (19, 7)

•  Components of interest: SV, Cycle 0, Cycle 1, Cycle 2 –  SV results: 48 (37 ,28) published papers

•  18 (14, 9) from NA, 20 (18,15) from Eu, 6 (2,2) from EA,1(0) Chile, 2(2) from Other (Mx)

–  Cycle 0 results: 164 (118, 41) published papers •  NA: 55 (26, 10) from 36 highest ranked projects and five fillers

–  Cycle 1 results: 22 (1,0) published papers •  NA: 9 published papers from 69 highest ranked projects

–  Cycle 2 results: 3 published papers, 1 from NA –  Some papers contain multiple ALMA data components


Early Science continued •  164 published papers from the 113 Cycle 0 high priority projects

–  55 published NA papers from deliveries of 38 projects –  Eu: 57 published papers from Cycle 0 deliveries of 35 projects –  EA: 34 published papers from Cycle 0 deliveries of 27 projects –  No refereed papers from 7 (26) Cycle 0 NA projects so far (several in final

stages of preparation)

•  19 published papers from 71 (0) Cycle 1 deliveries of 198 projects –  NA: 8 published papers from 30 deliveries of 69 highest ranked projects –  Eu: 9 published papers from 22 deliveries of 54 highest ranked projects –  EA: 2 published papers from 12 deliveries of 50 highest ranked projects

•  3 published papers from 36 (0) Cycle 2 deliveries of 355 projects –  NA: 1 published paper from 19 (0) Cycle 2 deliveries of 118 projects –  Eu: 2 published papers from 10 Cycle 2 deliveries of 116 projects –  EA: 0 published papers from 2 deliveries of 83 projects.


ALMA Publication Data Source Archival vs PI data

•  Archive


ALMA Archive Dataflow In from AOS, out through ARCs

•  Increase in outflow


ALMA/NA Papers Summary

•  ALMA publications continue to rise rapidly –  Number has doubled in past year –  Citations have tripled –  Large (~6x) increase in NRAO telescope user community –  Increasing use of archival data

•  Papers from all three cycles are being produced by NA authors at about the same rate as in other Executives, proportionally

•  NAASC and JAO are well-represented among authors on papers.


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science overview & publications · • cycle 1: jan 2013-may 2014 (1131 proposals, 800h): –...

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