MAORY science team activity Giuliana Fiorentino (INAF-OABo) 1 on - - PowerPoint PPT Presentation

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MAORY science team activity Giuliana Fiorentino (INAF-OABo) 1 on - - PowerPoint PPT Presentation

Sep 30, 2023 178 likes •486 views

MAORY science team activity Giuliana Fiorentino (INAF-OABo) 1 on behalf of the MAORY consortium Friday, May 26, 2017 MAORY, the PROJECT the first light AO module for E-ELT providing a diffraction limit for a 39-m telescope Designed and to be

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MAORY science team activity

Giuliana Fiorentino (INAF-OABo)

  • n behalf of the MAORY consortium

1 Friday, May 26, 2017

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Designed and to be build by a consortium including several INAF Institutes (OA-Bo, IASF-Bo, OA-Arcetri, OAPd, OA-Na, OA-Brera) + INSU-IPAG-Grenoble SCAO mode: high Strehl correction Over a D~10” FoV with one bright NGS (7≤V≤16) MCAO mode: moderate but homogeneous Strehl correction over a D~180” FoV with 3 NGS (H≤19) + 6 LGS MAORY will feed the high resolution imager MICADO (that will include a spectrographic mode) The SCAO module is a joint project with MICADO consortium MAORY will be integrated at the IASF-Bologna labs

MAORY PI: Emiliano Diolaiti MAORY PM: Paolo Ciliegi

MAORY, the PROJECT the first light AO module for E-ELT providing a diffraction limit for a 39-m telescope

2 Friday, May 26, 2017

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Designed and to be build by a consortium including several INAF Institutes (OA-Bo, IASF-Bo, OA-Arcetri, OAPd, OA-Na, OA-Brera) + INSU-IPAG-Grenoble SCAO mode: high Strehl correction Over a D~10” FoV with one bright NGS (7≤V≤16) MCAO mode: moderate but homogeneous Strehl correction over a D~180” FoV with 3 NGS (H≤19) + 6 LGS MAORY will feed the high resolution imager MICADO (that will include a spectrographic mode) The SCAO module is a joint project with MICADO consortium MAORY will be integrated at the IASF-Bologna labs

MAORY PI: Emiliano Diolaiti MAORY PM: Paolo Ciliegi

MAORY, the PROJECT the first light AO module for E-ELT providing a diffraction limit for a 39-m telescope

2

low sky coverage!

Friday, May 26, 2017

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Designed and to be build by a consortium including several INAF Institutes (OA-Bo, IASF-Bo, OA-Arcetri, OAPd, OA-Na, OA-Brera) + INSU-IPAG-Grenoble SCAO mode: high Strehl correction Over a D~10” FoV with one bright NGS (7≤V≤16) MCAO mode: moderate but homogeneous Strehl correction over a D~180” FoV with 3 NGS (H≤19) + 6 LGS MAORY will feed the high resolution imager MICADO (that will include a spectrographic mode) The SCAO module is a joint project with MICADO consortium MAORY will be integrated at the IASF-Bologna labs

MAORY PI: Emiliano Diolaiti MAORY PM: Paolo Ciliegi

MAORY, the PROJECT the first light AO module for E-ELT providing a diffraction limit for a 39-m telescope

2

low sky coverage! high sky coverage!

Friday, May 26, 2017

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5 mas = 0.005” 10 mas = 0.010” 50 mas = 0.050” ELT Spatial Resolution: ~6 times better than JWST

0.6 pc @ D=10 Mpc

MAORY-MCAO mode: the sky coverage machine! SC≥50% in everywhere, ~100% for b < 30˚

3 Friday, May 26, 2017

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5 mas = 0.005” 10 mas = 0.010” 50 mas = 0.050” ELT Spatial Resolution: ~6 times better than JWST

0.6 pc @ D=10 Mpc

MAORY-MCAO mode: the sky coverage machine! SC≥50% in everywhere, ~100% for b < 30˚

wavelength range

3 Friday, May 26, 2017

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5 mas = 0.005” 10 mas = 0.010” 50 mas = 0.050” ELT Spatial Resolution: ~6 times better than JWST

0.6 pc @ D=10 Mpc

MAORY-MCAO mode: the sky coverage machine! SC≥50% in everywhere, ~100% for b < 30˚

wavelength range

JWST =27.9 JWST =38.7 JWST =51.7 JWST =69.8 3 Friday, May 26, 2017

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5 mas = 0.005” 10 mas = 0.010” 50 mas = 0.050” ELT Spatial Resolution: ~6 times better than JWST

0.6 pc @ D=10 Mpc

MAORY-MCAO mode: the sky coverage machine! SC≥50% in everywhere, ~100% for b < 30˚

wavelength range

3 Friday, May 26, 2017

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There is also a coronographic mode Large- Pixel Scale=4 mas/px Nyquist sampling H,K Narrow- Pixel Scale=1.5 mas/px Nyquist sampling down to I

Feeding MICADO: the imager

4

from the MICADO Operational Concept Description

Friday, May 26, 2017

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Astrometric requirements for the E-ELT

ASTROMETRY of internal proper motions in: p.m. (mas/yr) = v(km/sec)/d (Kpc) * 0.206265 Globular clusters at 50Kpc and v~10Km/sec -> 40μas/yr, in 5 yr for a sample of > 100 stars the relative accuracy is 50 μas/(200 μas*√100) = 2% Dwarf galaxies at 1Mpc and v~10Km/sec -> 2μas/yr, in 10 yr for a sample of >100 stars, the relative accuracy is 50 μas/(20 μas*√100) = 20% the requirement is an astrometric precision of 50 μas (goal 10 μas) on bright stars 20x20 MICADO FoV. p r

  • p

e r m

  • t

i

  • n

~ 4 μ a s / y r v~10Km/Sec

d~50Kpc

5 Friday, May 26, 2017

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60”

ground - 2.5m

preparing the era for ELTs

NGC4470 in Virgo distance~17 Mpc

6

Friday, May 26, 2017

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60”

ground - 2.5m

preparing the era for ELTs

30”

H S T

  • 2

. 4 m

NGC4470 in Virgo distance~17 Mpc

6

Friday, May 26, 2017

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60”

ground - 2.5m

preparing the era for ELTs

30”

H S T

  • 2

. 4 m

3”

E-ELT - 39m

NGC4470 in Virgo distance~17 Mpc

Deep, Fiorentino et al. 2011

6

Friday, May 26, 2017

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Photometric requirements for the E-ELT into the crowd of ELLIPTICALs

“The ultimate goal is to study the resolved stellar populations in giant elliptical galaxies, of which there is no example in the LG, and we have to look at Cen A to find the closest example of a peculiar elliptical. However, the best place to look at the properties of a range of elliptical galaxy types is the Virgo cluster which contains thousands of large galaxies and tens of giant ellipticals of a range of size and position in the

  • cluster. Of particular interest are the crowded central regions of galaxies where most of the stellar mass lies.”

Deep, Fiorentino, et al. 2011

The requirement is a photometric precision of few 0.01 mag over the full MICADO FoV.

PHOTOMETRY of Elliptical galaxies:

7 Friday, May 26, 2017

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MAORY Science Team

  • Definition of MAORY+MICADO

Science Cases

  • Definition of the scientific drivers

constraining MAORY (+MICADO) final design

  • To provide support to the technical

team in defining and fulfilling specifications

  • To prepare the exploitation of the ELT

GTO awarded to INAF for building MAORY: 54 E-ELT nights (MICADO +HARMONI) Chair: M. Bellazzini (INAF-OA Bo) Deputy: G. Fiorentino (INAF-OA Bo)

  • P. Ciliegi (INAF-OA Bo)
  • E. Maiorano (INAF-IASF Bo)
  • F. Mannucci (INAF-OA Arcetri)
  • M. Mapelli (INAF-OA Pd)
  • P. Saracco (INAF-OA Brera)
  • M. Spavone (INAF –OA Na)
  • S. Douté (IPAG)
  • G. Chauvin (IPAG)

Started activity in phase B, kick off February 2, 2016 (2 meetings so far)

8

TB extended!!

Friday, May 26, 2017

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We want you

MAORY Science Cases: assembling the MAORY SC book

9

  • n February 28 we made a call for

science cases to all the INAF institutes

Friday, May 26, 2017

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We want you

MAORY Science Cases: assembling the MAORY SC book

9

  • n February 28 we made a call for

science cases to all the INAF institutes

Friday, May 26, 2017

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MAORY Science Cases: assembling the MAORY SC book Take what you need:

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24 ‘resolved’ 18 ‘unresolved’

1 Osservatorio di Torino 2 Osservatorio di Brera 3 IASF Milano 4 Osservatorio di Padova 5 Osservatorio di Trieste 6 Osservatorio di Bologna 7 IRA Bologna 8 IASF Bologna 9 Osservatorio di Arcetri (FI) 10 Osservatorio di Teramo 11 Osservatorio di Roma 12 IAPS Roma 13 Osservatorio di Capodimonte (NA) 14 Osservatorio di Cagliari 15 Osservatorio di Palermo 16 IASF Palermo 17 Osservatorio di Catania

Friday, May 26, 2017

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MAORY Science Cases: assembling the MAORY SC book Take what you need:

10

24 ‘resolved’ 18 ‘unresolved’

1 Osservatorio di Torino 2 Osservatorio di Brera 3 IASF Milano 4 Osservatorio di Padova 5 Osservatorio di Trieste 6 Osservatorio di Bologna 7 IRA Bologna 8 IASF Bologna 9 Osservatorio di Arcetri (FI) 10 Osservatorio di Teramo 11 Osservatorio di Roma 12 IAPS Roma 13 Osservatorio di Capodimonte (NA) 14 Osservatorio di Cagliari 15 Osservatorio di Palermo 16 IASF Palermo 17 Osservatorio di Catania

Friday, May 26, 2017

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Collected MAORY Science Cases

11

9/17 INAF Institutes so far replied to the MAORY SC call

5% 7% 7% 2% 19% 21% 23% 14% 2% OATo OABrera OAPD OABo OAArcetri OATe OARoma OAC IASF-Bo

Friday, May 26, 2017

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Collected MAORY Science Cases

11

9/17 INAF Institutes so far replied to the MAORY SC call

5% 7% 7% 2% 19% 21% 23% 14% 2% OATo OABrera OAPD OABo OAArcetri OATe OARoma OAC IASF-Bo

Friday, May 26, 2017

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Collected MAORY Science Cases

12

44% 56% Resolved Ma2-Ma3 Unresolved Ma1-Ma4

more science cases are likely to be collected...

Friday, May 26, 2017

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Required MAORY observing modes

13

so far MAORY SC mainly require the imaging mode

10% 20% 12% 59% IMAGING ASTROMETRY SPECTROSCOPY IMA-SPC IMA-ASTR

Friday, May 26, 2017

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Required AO observing modes

14

so far MAORY SC mainly require the imaging mode

24% 10% 66% MCAO SCAO SCAO/MCAO

Friday, May 26, 2017

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Required FoV/ Pixel scale

15

so far MAORY SC mainly require the imaging mode

1.5/4mas/px 17% 4mas/px 54% 1.5mas/px 29% 1.5mas/px 4mas/px 1.5/4mas/px

20”x20” 50”x50”

Friday, May 26, 2017

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Focus on resolved stellar populations

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Compact star clusters within our galaxy dark matter content of old and young clusters (astrometry & photometry)

  • rigin of multi pop in GCs

(astrometry & photometry) Bulge formation and evolution (photometry) Young stars Jets characterization and disk/accretion interaction (narrow band photometry) Search for proto-planets (≥ 1

MJup ) in proto-planetary disks

(photometry)

Friday, May 26, 2017

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SLIDE 27

Focus on resolved stellar populations

17

Compact star clusters beyond the MW Nuclear Star Clusters in 30 Doradus (astrometry & photometry) Nuclear Star Clusters beyond the Local Group (photometry & spectroscopy) GCs as age and metallicity stellar tracers (photometry & spectroscopy) IMF in low metallicity environments (photometry) Star Formation in merged galaxies (photometry)

Friday, May 26, 2017

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Focus on resolved stellar populations

18

Galaxies beyond the Local Group Galaxies formation and evolution with stellar ages and metallicity (photometry & spectroscopy) Distance scale with primary and secondary indicators (photometry & spectroscopy) Obscured galaxies in ZOA (photometry)

Friday, May 26, 2017

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next steps...

  • Interaction with PI-s in particular to help with the technical form and to

suggest possible merge;

  • Detailed simulations (SCAO PSFs are already available, MCAO coming

soon), so far are mainly based on Phase-A study;

  • next meeting within autumn 2017;
  • White book assembling, authorship will be recognized and properly

advertised (on astro-ph);

  • February 2 2018, end of Phase-B activity.

19 Friday, May 26, 2017

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Thanks!

20 Friday, May 26, 2017