IYAS 2015 NOEMA. the NOrthern Extended Millimeter Array. K.F. Schuster - IRAM

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1 NOEMA IYAS 2015 the NOrthern Extended Millimeter Array K.F. Schuster - IRAM

2 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

3 30 m Telescope Spain Interferometer PdB/NOEMA, France Headquarter Grenoble, France

4 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. IRAM Plateau de Bure NOEMA NOEMA & ALMA ALMA

5 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 CARMA Comparison of Collecting Area [m 2 ] Interferometry NOEMA SMA Total Power and Short Spacing ALMA ALMA NOEMA/30m

6 Sensitivity Goals Continuum or Frequency Survey Single Line NOEMA vs ALMA > 55% > 35%

7 Imaging 100 GHz J Boissier 2009 M31 (GALEX) PdBI AB Conf 0.88 x x 0.90

8 Imaging 100 GHz M31 (GALEX) NOEMA Ext Conf 0.88 x x 0.46 resolve GMCs in Virgo

9 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

10 Science with PdBI/NOEMA ALMA 0.45 mm PdBI 1.3 mm GG Tau circumbinary disk (Dutrey et al Nature)

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13 1 = 2.4 kpc PdBI Map of CO(1-0) in M51 PdBI ABCD 1.1 Schinnerer (PI), Dumas, Garcia-Burillo, Kramer, Leroy, Meidt, Pety, Rix, Schuster, Thompson

14 Science with PdBI/NOEMA C+ in J at z=7.08 (Venemans et al. 2012) CII C+ in HFLS3 at z =6.34 (Riechers et al. 2013)

15 NOEMA - Poking in the redshift Space Chapman et al 2015

16 NOEMA - Galactic Molecular Outflows SDSSJ Geach, J.E., Nature - December 4 Volume 516; Cicone et al. 2014, A&A, 562, A21

17 Science with PdBI/NOEMA PHIBSS & PHIBSS-2 surveys of CO(3-2) in z =1-2 galaxies (Tacconi et al. 2013)

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19 LP T0CC PI J-P.Kneib 6 cluster mm Pushing the Luminosity Function

20 The Antenna

21 The NOEMA Receivers NOEMA RF Band Specifications Band NOEMA-1 NOEMA-2 NOEMA-3 NOEMA-3 RF Frequency (GHz)

22 NOEMA receivers

23 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 F Lo USB 4 GHz 12 GHz

24 NOEMA Special Features I Backend POLYFIX NOEMA backend will provide simultaneously: a) full continuum sensitivity, 8 G Hz 8 G Hz b) a large number of flexible high resolution windows. 8 G Hz With >4 Bit NOB the backend achieves 98% efficiency at all times. 8 G Hz 8 G Hz 4 G Hz 4 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!!! SURVEY BASE MODE 2 x 16 flex. Windows 64 MHz/62KHz res. 4 G Hz 4 G Hz 4 GHz / 0.25 MHz res. 4 GHz / 0.25 MHz res. 4 GHz / 2 MHz res. 4 GHz / 2 MHz res. 8 G Hz

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

26 GHz 400 Redshifted CO, CII and OI transitions CII OI B Line distance <23 GHz B B B redshift z

27 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-beworked-on option.

28 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

29 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

30 Antenna 7 inauguration 22 Sept. 2014

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33 Imaging with NOEMA7 Extreme star formation in galaxies merger (Koenig et al. 2015)

34 8 th NOEMA Antenna 4 days ago

35 Preparation of 9 th Antenna

36 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.

37 EMIR, the worlds most powerful mm wave receiver (produces up to 64 GHz of IF band) K.F. Schuster IRAM

38 EMIR receiver 16 GHz per polarization already available with EMIR (30 m) EMIR tests 2012 Lefloch et al. 2013

39 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 Sens. 2.0 mm = 11 mjy/sqrt(hz) Sens. 1.3 mm = 15 mjy/sqrt(hz)

40 NIKA 2 (PI Benoit et Monfardini) 6 FOV KID Camera Dual band mm Polarimetry Commissioning started 6 weeks ago

41 NIKA 2 Commissioning NGC 891

42 New Heterodyne Multibeam Receivers for the 30m Prototype 3mm dual pol Subsection Layout of 49 Pixel 1.3mm Array

43 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 8 th 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

44 NOEMA (Northern Extended Millimeter Array) Thank You for Your Attention