science overview & publications · • cycle 1: jan 2013-may 2014 (1131 proposals, 800h): –...
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Al Wootten
Science Overview & Publications
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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
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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
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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
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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
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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
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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)
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SDP.81 at z = 3.04
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ALMA Partnership, Vlahakis et al. 2015
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The Long Baseline Campaign: SDP.81 at z=3.04
ALMA Partnership, Vlahakis et al. 2015 0.01”= 400 pc at z=3
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Revealing the Complex Nature of SDP.81
Dye et al. 2015 (see also Rybak et al.)
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Long Baseline Campaign: HL Tau
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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
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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)
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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
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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.
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ALMA Publication Data Source Archival vs PI data
• Archive
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ALMA Archive Dataflow In from AOS, out through ARCs
• Increase in outflow
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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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