NOEMA the

NOrthern Extended Millimeter Array

K.F. Schuster - IRAM

IYAS 2015

IRAM Organization

• Founded 1978 CNRS (France)

MPG (Germany),

ING (Spain) joins 1989

• HQ Grenoble Admin., Technical Dev. (75 (~70 Pers.) Pers.) Softw. & Data Center

• Observatories: Pico Veleta (Spain)

(~50 Pers.) Plateau de Bure (France)

• Annual Budget 14 Mio. EU

Headquarter Grenoble, France

Interferometer PdB/NOEMA, France

30 m Telescope Spain

Advanced Millimeter Wave Astronomy calls: • for an ALMA competitive equivalent on the northern hemisphere • for an instrument which allows for large surveys. • for an observatory which allows the IRAM community to efficiently prepare and complement ALMA observations.

Panoramic winter view of the Plateau de Bure observatory as seen from southwest. The antennas are arranged in the intermediate C-configuration. In the background are the hangar and the living quarters. Credit: A.Rambaud / IRAM.

IRAM Plateau de Bure NOEMA

NOEMA

& ALMA

ALMA

NOEMA Northern Extended Millimeter Array

•Double the number of 15 m antennas at PdB from 6 to 12 •Increase of IF bandwidth from 8 GHz to 32 GHz •Extension of the Baselines from 0.8 to 1.6 km Comparison of Collecting Area

[m2]

Interferometry Total Power

and Short Spacing

ALMA 5655 914

NOEMA/30m 2121 707

SMA

CARMA

ALMA

NOEMA

Sensitivity Goals

Continuum

or

Frequency Survey

Single Line

NOEMA

vs

ALMA > 55% > 35%

0.88” x 0.73” 1.06” x 0.90”

M31 (GALEX) PdBI AB Conf

Imaging Simulations @ 100 GHz

J Boissier 2009

Imaging Simulations @ 100 GHz

0.88” x 0.73” 0.62” x 0.46”

M31 (GALEX) NOEMA Ext Conf

resolve GMCs in Virgo

NOEMA Science • Investigate Galaxy- and Star Formation

throughout the history of the universe.

• Understand interstellar chemistry and its influence on star and planet formation – what is the chemical heritage and potential impact on emergence of life ?

• Allow large, statistically significant surveys

• Provide easy accessible discovery space

• Generate full sky coverage in the millimeter range.

• Enhance IRAM partners use of ALMA

Science with PdBI/NOEMA

ALMA 0.45 mm

PdBI 1.3 mm

GG Tau circumbinary disk (Dutrey et al. 2015 Nature)

PdBI Map of CO(1-0) in M51

Schinnerer (PI), Dumas, Garcia-Burillo, Kramer, Leroy, Meidt, Pety, Rix, Schuster, Thompson

1’ =

2.4

kp

c

PdBI ABCD 1.1”

CII

C+ in J1120+06 at

z=7.08

(Venemans et al. 2012)

Science with PdBI/NOEMA

C+ in HFLS3 at z =6.34 (Riechers et al. 2013)

Chapman et al 2015 NOEMA - Poking in the redshift Space

Cicone et al. 2014, A&A, 562, A21 Geach, J.E., Nature - December 4 Volume 516;

SDSSJ0905+57

NOEMA - Galactic Molecular Outflows

Science with PdBI/NOEMA

PHIBSS & PHIBSS-2 surveys

of CO(3-2) in z =1-2 galaxies

(Tacconi et al. 2013)

LP T0CC PI J-P.Kneib 6 cluster 90 hr @ 1.2mm

Pushing the Luminosity Function

The Antenna

The NOEMA Receivers

NOEMA RF Band Specifications

Band NOEMA-1 NOEMA-2 NOEMA-3 NOEMA-3

RF Frequency

(GHz) 72-116 127-179 200-276 275-373

NOEMA receivers

New 8 GHz 2SB Technology Since summer 2013 commissioned in all 4 bands in

EMIR, newest version is fully integrated

Delivers 16 GHz of IF band per polarization !

LSB USB

4 GHz 12 GHz

FLo

NOEMA Special Features I

Backend POLYFIX

• NOEMA backend will provide simultaneously:

a) full continuum sensitivity,

b) a large number of flexible high resolution windows.

With >4 Bit NOB the backend achieves 98% efficiency at all times.

8 G Hz 8 G Hz

8 G Hz 8 G Hz

4 G Hz 4 G Hz

2 x 16 flex. Windows 64 MHz/62KHz res.

4 GHz / 2 MHz res. 4 GHz / 2 MHz res.

BASE MODE

4 G Hz 4 G Hz 4 GHz / 0.25 MHz res. 4 GHz / 0.25 MHz res.

SURVEY MODE

8 G Hz 8 G Hz

8 G Hz 8 G Hz

8 G Hz 8 G Hz

8 G Hz 8 G Hz

32 GHz full Coverage in 2 Tunings !!!

Fast Sampling for 4 GHz Sub-bands (Gentaz et al.)

0

50

100

150

200

250

300

350

400

0 1 2 3 4 5 6 7

redshift z

GH

z

B1

B2

B3

B4

1-0

2-1

3-2

4-3

5-4

6-5

7-6

Line distance <23 GHz

Redshifted CO, CII and OI transitions

CII OI

NOEMA Special Features II

• NOEMA will allow efficient self calibration for sources as weak as 2 mJy at 3mm and 5 mJy at 1.3 mm.

• NOEMA continuum observations will allow for many sources spectral index measurements and multifrequency synthesis.

• Polarimetry as a hardware prepared to-be-

worked-on option.

Next Steps and future NOEMA Enhancements

•Full Phasing for VLBI (funded, in preparation) •Dichroic Mirrors and second Polyfix backend for full polarization Dual Band Observations (reference distribution installed, funded, design study started)

•Full Stokes Polarimetry

•Multibeam Receivers for Interferometry

Project Status Planning

The Project has been split into two Phases: Phase I: +4 Antennas + Receivers + Correlator for 12 Antennas Phase II: + 2 Antennas + Receivers + Baseline Extension

Phase I (34 MEu) is currently underway, constr. ends 2017 Phase II (15 MEu) needs identification of additional resources or/and new partners and ideally is following Phase I without gap. Until 2019

Antenna 7 inauguration 22 Sept. 2014

Imaging with NOEMA7

Extreme star

formation in

galaxies merger

(Koenig et al.

2015)

8th NOEMA Antenna 4 days ago

Preparation of 9th Antenna

The IRAM 30m Telescope Status and Future Evolution

• EMIR with high resolution

backends for up to 64 GHz total bandwidth

• GISMO and NIKA the continuum path finder instruments

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

• The 50 pixel 3mm Heterodyne array

• SHERA the 98 Pixel successor of HERA at 1.3 mm.

K.F. Schuster IRAM

EMIR, the worlds most powerful mm wave receiver

(produces up to 64 GHz of IF band)

EMIR receiver

Lefloch et al. 2013 EMIR tests 2012

16 GHz per polarization – already

available with EMIR (30 m)

NIKA I (Neel IRAM KID Array) a small dual band KID path finder camera

for 2 & 1 mm

S1.2mm=30mJy+-2mJy

Sens. 2.0 mm = 11 mJy/sqrt(Hz) Sens. 1.3 mm = 15 mJy/sqrt(Hz)

(z=3.93)

NIKA 2 (PI Benoit et Monfardini) 6’ FOV KID Camera Dual band 2 + 1.3 mm Polarimetry

Commissioning started 6 weeks ago

NIKA 2 Commissioning NGC 891

New Heterodyne Multibeam Receivers for the 30m

Prototype 3mm dual pol Subsection

Layout of 49 Pixel 1.3mm Array

Summary / Conclusions

•After developing the post ALMA technology, IRAM has started NOEMA construction employing this technology.

•NOEMA will provide an unique tool for European astronomers. •NOEMA saw “first light” in early 2015 (Ant 7) with the following big step in 2016 when the 8th Antenna and the correlator PLOYFIX will be commissioned.

•The synergy between NOEMA, the upgraded 30m and ALMA will be very high. •The flexible character and performance of NOEMA and the 30m telescope will guarantee unique discovery space and at the same time enable groundbreaking survey programs.

•Political efforts concentrate now on organizing Phase 2

NOEMA (Northern Extended Millimeter Array)

Thank You for Your Attention