1. ALMA Capacities for Spectral Line Emission
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
ALMA Capacities for Spectral Line Emission
Al Wootten
ALMA Interim Project Scientist
NRAO
As someone in a 50+ configuration myself…
Science with ALMA -- a new era for astrophysics

2. Boom Time for IS Spectroscopy
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Boom Time for IS Spectroscopy
Correlator technology: Huge increases in data processing ability produce a flood of new data
Telescopes: GBT combines collecting area with powerful correlator capacity: 8 new molecules in the past 2 yrs, nearly complete coverage to 50 GHz, 90GHz tests good.
All-sky: AT, ASTE, NANTEN II, APEX in the S. hemisphere, soon to be followed by ALMA
Multibeaming: NRO 45M, FCRAO, JCMT, APEX, LMT
Interferometers: No longer limited in spectroscopic capability, new and upgraded instruments (CARMA, IRAM) improve bandwidth and sensitivity

3. Hundreds of Spectral Lines
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Hundreds of Spectral Lines
Kaifu, et al., TMC-1, 2004.
Nobeyama spectral scan.
414 lines (8 to 50 GHz)
38 species.
Some likely to show Zeeman splitting.
“D-array” EVLA
Resolution,
Spectral baseline stability,
Imaging.
EVLA can observe 8 GHz at one time – an average of 80 lines --- at 1 km/s velocity res’n (30 GHz)
EVLA Correlator can “target” many (~60) lines at once.
8 GHz
TA*

4. MUSTANG: 90 GHz Imaging Array for the GBT
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Upenn: S. Dicker, P. Korngut, M.Devlin (PI)
GSFC: D.Benford, J.Chervenak, H. Moseley, J. Staguhn, S.Maher,T. Ames, J. Forgione
NIST: K.Irwin
NRAO: M.Mello, R.Norrod, S.White, J.Brandt, B.Cotton

5. Product Assurance
4/21/ June 2 – 6, Victoria, Canada
EVLA: J1148
VLA
VLA: A Single integration resulted in a two point spectrum, 43 MHz resolution, several needed for line profile (and to discover the correct z!).
EVLA:
Single integration covers up to 8 GHz (5.1 GHz shown, 10 MHz resolution)
Single integration covers the entire 870 micron ‘Band’ as seen from beneath Earth’s atmosphere.
EVLA II (not funded) brings ‘E’ array for short spacings.
CO 3-2
HCN3-2
HCO+ 3-2

6. ALMA Receivers/Front Ends
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
ALMA Receivers/Front Ends
NAOJ ?
SRON
NAOJ
IRAM
NRAO
6 units EU ?
HIA
Not assigned
Responsible
SIS
HEMT
Receiver technology
787 – 950 GHz
602 – 720 GHz
385 – 500 GHz
275 – 373 GHz*
211 – 275 GHz
GHz
125 – 169 GHz
84 – 116 GHz
67 – 90 GHz
31.3 – 45 GHz
Frequency Range
DSB
345 K
230 K 10
263 K (150K)
175 K (120K) 9
2SB
147 K
98 K 8
221 K (90K)
147 K (80K) 7
138 K (60K)
83 K (40K) 6
108 K
65 K 5
85 K
51 K 4
62 K (50K)
37 K (35K) 3
LSB
50 K
30 K 2
USB
28 K
17 K 1
Mixing scheme
TRx at any RF frequency
TRx over 80% of the RF band
Receiver noise temperature
ALMA
Band
Dual, linear polarization channels:
Increased sensitivity
Measurement of 4 Stokes parameters
183 GHz water vapour radiometer:
Used for atmospheric path length correction

7. Passband taken with ALMA Band 6 mixer at the SMT
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Passband taken with ALMA Band 6 mixer at the SMT
Ziurys has shown a SgrB2(N) spectrum at the American Chemical Society meeting in Atlanta, obtained with an ALMA prepreproduction B6 front end on the SMT. This system achieved 107 K system temperature, SSB at 45 deg. elevation at 232 GHz, with > 20 db image rejection, good baselines.

8. Summary of current status
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Summary of current status
Frequency
30 to 950 GHz: B3, B6, B7, B9 receivers passed CDR & PAI, preproduction units available, all meet Trx spec, most exceed specs. B6 tested on SMT.
Bandwidth
8 GHz both polzns, fully tunable: All units
Spectral resolution
31.5 kHz (0.01 km/s) at 100 GHz: 1st quadrant built
Angular resolution
30 to 0.016” at 300 GHz: Configuration defined
Dynamic range
10000:1 (spectral); 50000:1 (imaging)
Flux sensitivity
0.2 mJy in 1 min at 345 GHz (median conditions)
Antenna complement
Up to 64 antennas of 12m diameter, plus compact array of 4 x 12m and 12 x 7m antennas (Japan): Contracts for 53 up to 67, three prototype antennas in hand meet all specifications

9. ALMA Observes the Millimeter Spectrum
Product Assurance
ALMA Observes the Millimeter Spectrum
4/21/ June 2 – 6, Victoria, Canada
COBE observations
Millimeter/submillimeter photons are the most abundant photons in the cosmic background, and in the spectrum of the Milky Way and most spiral galaxies.
Most important component is the 3K Cosmic Microwave Background (CMB)
After the CMB, the strongest component is the submm/FIR component, which carries most of the remaining radiative energy in the Universe, and 40% of that in for instance the Milky Way Galaxy.
ALMA range--wavelengths from 1cm to 0.3 mm, covers both components to the extent the atmosphere of the Earth allows.
Include diagram of the cosmic background spectrum xray thru radio
Perhaps that of the MW Galaxy??
Could show where mm/submm lies in em spectrum
ALMA’s wavelength range--a few human hairs to a stack of five dimes.

10. Highest Level Science Goals
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Highest Level Science Goals
Bilateral Agreement Annex B:
“ALMA has three level-1 science requirements:
The ability to detect spectral line emission from CO or C+ in a normal galaxy like the Milky Way at a redshift of z = 3, in less than 24 hours of observation.
The ability to image the gas kinematics in a solar-mass protostellar/ protoplanetary disk at a distance of 150 pc (roughly, the distance of the star-forming clouds in Ophiuchus or Corona Australis), enabling one to study the physical, chemical, and magnetic field structure of the disk and to detect the tidal gaps created by planets undergoing formation.
The ability to provide precise images at an angular resolution of 0.1". Here the term precise image means accurately representing the sky brightness at all points where the brightness is greater than 0.1% of the peak image brightness. This requirement applies to all sources visible to ALMA that transit at an elevation greater than 20 degrees. These requirements drive the technical specifications of ALMA. “
A detailed discussion of them may be found in the new ESA publication Dusty and Molecular Universe on ALMA and Herschel.

11. General Science Requirements
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
General Science Requirements
General Science Requirements, from ALMA Project Plan v2.0:
“ALMA should provide astronomers with a general purpose telescope which they can use to study at a range of angular resolutions millimeter and submillimeter wavelength emission from all kinds of astronomical sources. ALMA will be an appropriate successor to the present generation of millimeter wave interferometric arrays and will allow astronomers to:
Image the redshifted dust continuum emission from evolving galaxies at epochs of formation as early as z=10;
Trace through molecular and atomic spectroscopic observations the chemical composition of star-forming gas in galaxies throughout the history of the Universe;
Reveal the kinematics of obscured galactic nuclei and Quasi-Stellar Objects on spatial scales smaller than 300 light years;
Image gas rich, heavily obscured regions that are spawning protostars, protoplanets and pre-planetary disks;
Reveal the crucial isotopic and chemical gradients within circumstellar shells that reflect the chronology of invisible stellar nuclear processing;
Obtain unobscured, sub-arcsecond images of cometary nuclei, hundreds of asteroids, Centaurs, and Kuiper Belt Objects in the solar system along with images of the planets and their satellites;
Image solar active regions and investigate the physics of particle acceleration on the surface of the sun.
No instrument, other than ALMA, existing or planned, has the combination of angular resolution, sensitivity and frequency coverage necessary to address adequately these science objectives.“

12. For <430 GHz, PWV=1.5mm;  >430 GHz, PWV=0.35mm
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Brightness Temperature Sensitivity 1 min, AM 1.3, 1.5mm, *0.35 PWV, 1 km/s
For <430 GHz, PWV=1.5mm;  >430 GHz, PWV=0.35mm

13. Product Assurance
4/21/ June 2 – 6, Victoria, Canada
The ALMA Correlators
NRAO Baseline Correlator (four quadrants for 64 antennas, BW: 8 GHz x 2; 2 bit sampling with limited 3 or 4 bit sampling)
First quadrant operating in NRAO NTC, to be retrofitted with Tunable Filter Bank enhancement (UBx)
Second quadrant being completed at NRAO NTC
First installation at AOS TB next year.
Detailed list of Observational Modes in ALMA Memo 556 (available at
ACA Correlator (NAOJ)
Critical review early December
But digitizer samples at 3 bits

14. Baseline Correlator Overview
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Baseline Correlator Overview
Observer may specify a set of disjoint or overlapping spectral regions, each characterized by
Bandwidth (31.25 MHz to 2 GHz)
Each 2 GHz baseband input (8 available) drives 32 tunable digital filters
Frequency (Central or starting)
Resolution (number of spectral points)
Number of polarization products: 1 (XX or YY), 2 (XX and YY) or 4 (XX, YY, XY, YX cross-polarization products)
Improved sensitivity options (4x4 bit correlation, or double Nyquist modes)
Temporal resolution depends upon mode (from 16 msec to 512 msec)
Simultaneous pseudo-continuum and spectral line operation

15. Multiple Spectral Line Windows
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Multiple Spectral Line Windows
Multiple spectral windows
Within the 2 GHz IF bandwidth
For modes with total bandwidth 125 MHz to 1 GHz
Useful for high spectral resolution observations of e.g. several lines within IF bandwidth (examples to be shown)
Multi-resolution modes
Simultaneous high and low resolution
Line core and line wings simultaneously
Planetary Observations
Outflow/Core Observations
As an ALMA goal is ease of use, the Observing Tool will guide the observer through the maze of spectral line possibilities

16. Some ALMA Spectroscopic Science
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Some ALMA Spectroscopic Science
Solar System
Atmospheres and venting on small bodies
Atmospheric structure of large bodies
Star Formation and GMCs in the Milky Way
Infall, Outflow and the formation of stars
Nearby Galaxies
Chemistry, organization of structure, evolution
The Evolution of Galactic Structure
The last few billion years
The Birth of Galaxies and the Early Universe
How did all this come to be anyway?

17. ALMA Design Reference Science Plan (DRSP)
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
ALMA Design Reference Science Plan (DRSP)
Goal: To provide a prototype suite of high-priority ALMA projects that could be carried out in ~3 yr of full ALMA operations
DRSP 1.0 finished December 2003;
>128 submissions received involving >75 astronomers
Review by ASAC members completed; comments included
(DRSP2.0) being updated now to include enhancements brought to project by Japan.
Reviews by SACs over coming months
Current version of DRSP on Website at:
New submissions continue to be added.

18. ALMA: Large Molecules Wavelength coverage Sensitivity to weak emission
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
ALMA: Large Molecules
Wavelength coverage
Sensitivity to weak emission
And small molecules
CF+ detection Neufeld et al H2D+/ D2H+.
Critical symmetric molecular ions undetectable owing to lack of rotational lines:
CH3+, C2H2+
Deuterium substitution asymmetrizes the molecule, giving it a small dipole moment (~0.3D) and hence rotational lines
Although the lines are very weak, ALMA is very sensitive.
Although the spectra are very sparse, ALMA covers a wide frequency range.
Line identification through detection of multiple isotopomers:
e.g. H2D+/ D2H+, CDH2+, CD2H+

19. Fountains of Enceladus
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Fountains of Enceladus
From the Solar System
From the atmospheres of planets
‘Weather’ on Venus, Mars, Jovian planets
~5km baseline provides 0”.05 at 300 GHz
Generally, planets are large with respect to an ALMA beam
Advantage of ALMA’s ability to collect complete spatial frequency data
To that of satellites and smaller bodies
Comets
Volcanism on Io, Search for Molecules from the Fountains of Enceladus
Even UB313 ‘Eris’ with its moon ‘Dysnomia’ easily resolved, Eris could be imaged.
See Wednesday session…
ALMA Beam

20. To chemically complex star-forming regions such as IRAS16293-2422
Product Assurance
To chemically complex star-forming regions such as IRAS
4/21/ June 2 – 6, Victoria, Canada
+ Submm continuum
 cm-l continuum
Outflow Shock Chemistry
Chandler, Brogan, et al. (2005)

21. Water masers in NGC1333 4B (north):
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
It Moves!
ALMA Beam
Water masers in NGC1333 4B (north):
A flow in motion
Each shock lasts <2 months
Any parcel of gas must be exposed to a succession of shocks
ALMA will reveal the complex chemical evolution of these shocks.
Excellent brightness temperature sensitivity
Excellent, near-VLBI, resolution.

22. Proper Motion and Structure of Shocks in Dense Clouds
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Proper Motion and Structure of Shocks in Dense Clouds
ALMA Beam
Water masers observed over four epochs encompassing 50 days (22 GHz, VLBA). Several of the masers define an arc structure about 5AU in length. This consistently moved at a rate of mas/day, or 13.6 km/s.
Including the radial velocity offset, a space velocity of 13.7 km/s is calculated at an inclination of 6 degrees from the plane of the sky.
These structures apparently represent water emission from interstellar shocks driven by the outflow from SVS13.
The tremendous brightness of water masers make them good tracers of motions in molecular gas on small scales. The Very Long Baseline Array (VLBA) provides beams of about one half milliarcsecond (0.17 AU) in size and can measure proper motions of about 10 km s-1 in the several days to weeks lifetime of a typical maser at a distance of 350 pc, the distance generally employed for NGC Observationally, masers occur within about 100 AU of their low luminosity driving source, and provide excellent signposts for the source of a flow, as well as good probes of the flow geometry and dynamics. The geometry of a flow and the physics of maser emission (produced along a tangential sight-line through the flow cocoon) conspire to result in a spread of radial velocity in a typical low mass maser source of only a few km s-1. A few Herbig-Haro objects have measured proper motions of as much as a few hundred km s-1; CO also shows very high velocities in this source--can the masers also show such high space velocities? Here we report VLBA observations toward the region of NGC1333 near SSV13, the driving source for the well-known Herbig-Haro objects HH7-11. Maser emission was observed over four epochs spaced interstitially by three weeks during late 1998, SSV13 is associated with the millimeter continuum SED Class I source SSV13A1. High resolution CO observations have secured the association of the flow with the continuum object on arc-second scales. A 1998 Aug 12 VLA observation places the blueshifted masers within 80 AU (0''.2) of the 2.7 mm position for A1 reported from BIMA. We report observations of two groups of masers, one redshifted by about 6 km s-1 and one blueshifted by about 2-3 km s-1, separated by about 100 AU in projected distance along position angle 21 degrees. Red masers were present only in the latter two epochs. During all epochs, an arclike structure was present with similar morphology; over time this structure moved relative to the southernmost blue maser toward the southeast, roughly along the position angle defined by the Herbig-Haro objects, with a proper motion of about 13 km s-1.
Both redshifted and blueshifted masers are clearly part of the same lobe of the flow; their observed Doppler shifts are artifacts of the opening angle of the flow. Our data suggest that the opening angle is about 10o. We measure lower expansion velocities and a wider opening angle than has been found in some other flows near Class 0 SED objects, perhaps indicating that the flows open and slow as they age.
Masers near SVS13; 1mas=0.34AU
Blue Epoch I, Green Epoch III, Blue Epoch IV
Wootten, Marvel, Claussen and Wilking

23. Structure of Nearby Galaxies
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Structure of Nearby Galaxies
2’.7
162 beams
HST
Example from D. Meier (NRAO) DRSP
IC342 12CO, 13CO, C18O J=21, HNCO J=109
Image 4'x4' field of view. PB=27", nyquist=11”
324 pointings
10 sensitivity goal disk emission
B6 (1.3mm) line rms: 0.06 K
2 mins per pointing
11 hours, multiple (~8) mosaics
1mm cont rms: 65 uJy/bm
Example correlator setup…

24. Extragalactic CO Setup
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Extragalactic CO Setup
Line CO
13CO
C18O
HNCO
Cont
Frequency
USB
LSB
LSB
LSB
4 GHz
USB&LSB
Resolution*
0.64 km/s
21 km/s
Window
Q1: 500 MHz
Q2: 500 MHz
Q3&4: 2 GHz
Channel decimation
To ~5 km/s
Excise lines
Spatial resolution 1”
(300m)

25. Spectrum of a Normal Galaxy
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Spectrum of a Normal Galaxy
Z=2 in this example
L(CO)1-0~5x108 Kkm/s pc2 ~L(CO)2-1
SCO2-1~.1mJy
But when did ‘Normal’ galaxies evolve?
LIR~2 x 10^10

26. LIRGs 0.4<z<1 LIR~5 LIR(MW) so L(CO)2-1~5 L(CO)1-0, MW
Product Assurance
MIPS15942, z=0.44
4/21/ June 2 – 6, Victoria, Canada
LIRGs 0.4<z<1
MIPS4644, z=0.67
LIR~5 LIR(MW) so L(CO)2-1~5 L(CO)1-0, MW
Tsys~100K SSB;
Line 1 reaches 1K/1min 5 km/s;
Continuum 1 reaches .07 mJy/1min
Could possibly measure CO in ~two dozen MIPS-detected LIRGS in UDF falling in this redshift range, one transit per source
‘Age’ Gyr; Scale kpc/beam
HST UDF
Should include HCN

27. J1148+5251: an EoR paradigm with ALMA
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
J : an EoR paradigm with ALMA
CO J=6-5
Wrong declination (though ideal for Madrid)! But…
High sensitivity
12hr 1 0.2mJy
Wide bandwidth
3mm, 2 x 4 GHz IF
Default ‘continuum’ mode
Top: USB, 94.8 GHz
CO 6-5
HCN 8-7
HCO+ 8-7
H2CO lines
Lower: LSB, 86.8 GHz
HNC 7-6
C18O 6-5
H2O 658GHz maser?
Secure redshifts
Molecular astrophysics
ALMA could observe CO-luminous galaxies (e.g. M51) at z~6.
If one placed CO 6-5 in the LSB, one would get the line of H2O and the 7-6 line of 13CO, in addition to several H2CO lines, in the USB.

28. ALMA into the EoR Spectral simulation of J1148+5251
Product Assurance
ALMA into the EoR
4/21/ June 2 – 6, Victoria, Canada
Spectral simulation of J
Detect dust emission in 1sec (5s) at 250 GHz
Detect multiple lines, molecules per band => detailed astrochemistry
Image dust and gas at sub-kpc resolution – gas dynamics! CO map at 0”.15 resolution in 1.5 hours CO
HCO+
HCN
CCH
If one placed CO 6-5 in the LSB, one would get the line of H2O and the 7-6 line of 13CO, in addition to several H2CO lines, in the USB.
N. B. Atomic line diagnostics
[C II] emission in 60sec (10σ) at 256 GHz
[O I] 63 µm at 641 GHz
[O I] 145 µm at 277 GHz
[O III] 88 µm at 457 GHz
[N II] 122 µm at 332 GHz
[N II] 205 µm at 197 GHz
HD 112 µm at 361 GHz

29. Bandwidth Compression
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Bandwidth Compression
Nearly a whole band scan in one spectrum
Did I draw this right? Shouldn’t there be two 4*(1+z) windowd with an 8*(1+z) hole in the center?
LSB
USB
Schilke et al. (2000)

30. Summary First antenna in Chile within a year
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
Summary
First antenna in Chile within a year
Site, electronics and collecting area provide sensitivity
Wide bandwidths combined with a flexible correlator provide spectral coverage
Multiple spectral lines quickly accessible
Large surveys possible (but large area surveys relatively slow)
Robust excitation, abundance analyses possible
Imaging of emission regions provides dynamical information

31. European ALMA News (www.eso.org),
Product Assurance
4/21/ June 2 – 6, Victoria, Canada
European ALMA News (
ALMA/NA Biweekly Calendar (
The Atacama Large Millimeter Array (ALMA) is an international astronomy facility. ALMA is a partnership between Europe, North America and Japan, in cooperation with the Republic of Chile. ALMA is funded in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC), in Europe by the European Southern Observatory (ESO) and Spain. ALMA construction and operations are led on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (AUI), on behalf of Europe by ESO, and on behalf of Japan by the National Astronomical Observatory of Japan.