NOEMA the Northern Extended PMO Nanjing Millimeter Array March 2017 K.F. Schuster IRAM • Structure and Organization of IRAM • NOEMA • IRAM 30m TlTelescope and its IItnstrumen ttitation Program • Things to come • Conclusions IRAM OOgarganizat atoion

• Founded 1978 CNRS (France) as non-profit MPG (Germany ), organization IGN (Spain) joins 1989

• HQ Grenoble Science Operation and (~ 75 Pers.) Technical Dev. Softw. & Data Center Admin.

• Observatories: Pico Veleta (Spain) (~50 Pers.) Plateau de B. (France)

• Annual Budget 14 Mio. EU (consolidated) IRAM Mission

• Operate two world class mm/submm observatories

– IRAM 30m telescope Pico Veleta Spain – NOEMA Northern Extended Millimeter Array

• Develop advanced technology for millimeter Astronomy and act as an center of excellence in this field.

• Develop the related science community and training of forthcoming generations of scientists. Interferometer NOEMA (8/12), France

30 m Telescope, Spain

Headquarter Grenoble, France IRAM users

15% open time, 85% IRAM partner .Countries: 43 Millimeter Wave Astronomy fundamentally changed during the last 15 years:

•Became important pillar of multi-wavelength Astronomy.

•Transition from single object projects to multi object surveys.

•Arrival of ALMA, a 1.3 billion Eu world wide project in the southern hemisphere. NOEMA Northern Extended Millimeter Array

The Concept •Double the number of 15 m antennas at PdB from 6 to 12

•Increase of IF band width from 8 GHz to 32 GHz

•New Correlator: Full low resolution coverage + 128 flexible high resolution windows

•Extension of the Baselines from 0.8 to 1.6 km

•Organ ize ~ 50 MEu for thi s ! NOEMA Motivations

• Investigate - and Formation throughout the history of the universe.

• Understand interstellar and circumstellar chemistry and its influence on star and planet formation. Detection of complex and potentially prebiotic molecules.

• Allow large, statistically significant surveys.

• Provide easy accessible discovery space.

• Generate full sky coverage in the millimeter range.

• Enhance IRAM partners use of ALMA. The High Redshift Universe

Exmp. Dust and Gas at z=6 .35

(a) ~0.3" maps of the 158‐μm continuum in HFLS3, (b) velocity integrated [CII] line emission, (c) isovelocity field and (d) velocity dispersion map obtained with the IRAM interferometer in A‐configuration, overlaid on a Keck/NIRC2 2.2‐μm adaptive optics image (rest‐frame UV/optical light). Work by Riechers et al. 2013, Nature, 496, 239 PdBI Map of CO(1CO(1--0)0) in M51 kpc

2.4

=

1’

PdBI ABCD  1.1”

ShiSchinnerer (PI), Dumas, GGiarcia‐Burill o, Kramer, Leroy, Meidt , PPtety, Rix, SShchus ter, Thompson

ALMA as a benchmark

Comparison of “ideal” Collecting Area

Total Power [m2] Interferometry and Short Spacing

ALMA/ACA 5655 914

NOEMA/30m 2121 707 Sensitivities

IF: •ALMA receivers would have as low noise as NOEMA receivers •ALMAs observingNOEMA efficiency Sensitivity would equal thatGoals of NOEMA •NOEMA w ould ha ve as muc h mm obs time as ALMA does •and the followingContinuum parameters apply: Single Line NOEMAor ALMA N-AntFrequency 11.5 Survey 42.5 Adiam 15 12 NpixNOEMA 1 1 BW 16 8 vs Corr eff 0990.99 > 65%0880.88 > 45% ALMA

This is not taking into account advantages of NOEMA through simultaneous correlator modes or future dual frequency operation ! Angular Resolutions

CARMA

SMA

NOEMA

ALMA Imaggging Simulations @100 GHz

M31 (GALEX) PdBI AB Conf

0.88”1.06” x 0.73”0.90” Imaggging Simulations @100 GHz

M31 (GALEX) NOEMA Ext Conf

0.88”0.62” x 0.73”0.46”

resolve GMCs in Virgo The NOEMA Antenna

<35 m rms The NOEMA Receivers

NOEMA RF Band Specifi cati ons Band NOEMA-1 NOEMA-2 NOEMA-3 NOEMA-3 RF Frequency 72-116 127-179 200-276 275-373 (GHz) NOEMA receivers NOEMA 8 GHz 2SB Technology Since summer 2013 commissioned in all 4 bands at the 30m tltelescope, newest version is fllfully iitntegrat tded

D. Maier et al. Delivers 16 GHz of IF band per polarization !

LSBFLo USB

4 GHz 12 GHz NOEMA Correlator Technology Fast Sampling for 4 GHz Sub-bands (Gentaz et al.) Backend Work Packages Content O. Gentaz

IF and TX Laser Control Board

LO1 Transport & Ctrl System LO1Ref HiQ Cable

IF Correlator Proc LO1 FFT

E/O O/E ADC

4-12GHz RTDA NOEMA Special Features

Backend POLYFIX

• NOEMA backend will provide simultaneously: a) full conti nuum sensi t iv ity, 8 G Hz b) a large8 numberG Hz 8 of G flexible Hz high resolution8 G Hz windows. 8 G 8 GHz Hz

With >4 Bit NOB the backend achieves 98% efficiency at all times.8 G Hz 8 G Hz 8 G Hz 8 G Hz 8 GHzG Hz 32 GHz full Coverage in 2 Tunings8 !!!GHzG Hz

SURVEYBASE MODE 2 x 16 flex. WiWin ddows 6464 MHMHz /62KH/62KHz re s. 4 G Hz 4 G Hz 4 GHz4 /G 0.25 Hz MHz res. 4 GHz4 G/ 0.25 Hz MHz res. 4 GHz / 2 MHz re s. 4 GHz / 2 MHz res. Redshifted CO, CII and OI transitions

400

350 OI 7-6 CII B4 300

250 6-5 B3 Line distance <23 GHz 5-4 200 GHz 434-3 150 B2 3-2

2-1 100 B1

50 1-0

0 01234567 redshift z Next Steps and future NOEMA Enhancements

•Dichroic Mirrors and second Polyfix backend for full polarization Dual Band Observations ((ufun dedbyeded by ext taodraordina ayry fu nds fro m MPG, re eeeference distribution installed, design study started)

•Full Phasing for mm-VLBI (funded, in preparation)

•Full Stokes Polarimetry

•Multibeam Interferometry NOEMA Project Schedule

2017: Phase I: 10 Ants + Rx + 1st Correlator for 12 Ants

2018: Baseline Extension to 1.6 km

2019: Phase II: 12 Antennas + Rx

2020: Rx Dual Band Upgrad e + 2nd CltCorrelator Antenna 7 inauguration 22 Sept. 2014 Feb 2015 Apr 2016

NOEMA8 ALMA35 Cy 3

OMC2-FIR4, SOLIS LP OMC2-FIR4, Ceccarelli Caselli & Ceccarelli, B1 2015.1.00261.S, B3 RMS = 0100.10 mJy/(3mJy/(35x2.5x2.7”) RMS = 0150.15 mJy/(2mJy/(29x2.9x2.0”) Ant 9 – status Jan 16 Ant 9 – Status May 2016 Ant 9 – Status Sept 2016 Ant 9 22 Nov 16 Ant 9 first roll out 3 days ago ANT 10 22. Nov 16

We are ready for Antenna 11 and 12 ! BdBand 1 ~ 6hf/k

+4 GHz +4 GHz

Band 2 ~ 5hf/k

+4 GHz +4 GHz 70‐80 GHz band offers .new discovery space Orion A‐IRC2 .deep molecular line surveys .firs t‐ever opportittunity to perform synthesis mapping (no ALMA) .NOEMA + 30m telescope to sample spatial scales down to 131.3”

NOEMA: .74.7 ‐80 GHz, Dec 01, 2016 .70.8‐80 GHz in 2017

IRC+10216 NOEMA vs ALMA Receiver Noise Comparison

(in two weeks from now all Antennas upgraded) The IRAM 30m Telescope Status and Future Evolution

• EMIR with high resolution backends for up to 64 GHz total bandwidth

• NIKA II, a dual band continuum imager with 6 arcmin FOV and polarization option.

• HERA the 18 pixel 1.3 mm HdHeterodyne Array

•Theeutue50pe3 future 50 pixel 3mm a ad98nd 98 pixel 1.3 mm Heterodyne Arrays HERA 18 Pixel Heter ody ne Receiv eer Instrument Design RF Components Mixer Design A. Karpov et al 1998, Int J I MMW 19 Heterodyne multibeam receiver HERA comes into age but still unbeaten for larggpe maps.

M33 LP finished,

Together with VLA HI and Herschel continuum bands unique data set in sensitivity and resolution

First time, diffuse low level CO emiiission in HI spi ilrals ditldirectly imaged in place other than .

Braine and Schuster et al Heterodyne Large Scale Mapping

Walter, Leroy et al. 46 EMIR, the worlds most powerful mm wave receiver (produces up to 64 GHz of IF band)

K.F. Schuster IRAM Blossoming Chemistry with the 30m /EMIR

Observed profiles and results of model fitting (red) of the 14N16O J=5/3‐3/2 Π+ (left) and Π‐ bands transitions observed towards IRC+10420. The ticks in the line below the profile shows for each species the location of the hyperfine transitions. Work by Quintana‐Lacaci et al. 2013, A&A, 560, L2

A 250 MHz slice of the 3mm spectrum observed towards Sgr B2(N) with the IRAM 30m telescope, with a best‐fit model (green) and the most relevant lines (blue). The full 3mm spectrum covers the 80 to 116 GHz range. Work by Belloche et al. 2013, 559, A47 First Real KID Applications NIKA I, Neel IRAM KID Array, a prototype millimeter wave camera for the IRAM 30m telescope, 2010 Cygn-X at 2mm wavelength

Aluminum lumped Element Resonators NIKA I (Neel IRAM KID Array) a small dual band KID path finder camera for 2 & 1 mm

(z=3 .93) S1.2mm =30mJy+ -2mJy NIKA 2 (PI Benoit et Monfardini) 6’ FOV KID Camera Dual band 2 + 1.3 mm including 1.3mm Polarimetry

Commissioning started Nov 2015 NIKA 2 Optical Layo ut NIKA 2 Examples of maps from Commissioning

NGC891 (run 1) RXJ1347‐1145 (run 4)

2mm

1mm

2mm

Preliminary NEFD: 8 ±3 mJy·√s @ 2.0 mm 30 ±5 mJy·√s @ 112.2 mm Ori KL

2mm In tensity L o g

1.1mm

Beam Map 1.1mm - Mars New Heterodyne Multibeam Receivers for spectroscopic Imaging Prototype 3mm dual pol Subsection

Layout of 49 Pixel 1.3mm Array Examples of Things to Come glycolaldehyde Biver et al, Obs Paris with IRAM 30m, Nature 2015 Meinert et al., Univ. Nice, Science 2016

The Next Big Thing: CtiCreating a world wide itinter ferome ter (mm‐VLBI) to image the in the center of our galaxy!

NOEMA (Nor thern Ext end ed Millime ter Array)

Thank You for Your Attention