logoFRIDA 
Science Drivers


The FRIDA Project

Instrument Overview

Science Drivers

IAC Contribution

IAC Project Team

Sky coverage with AO with natural or laser guide star

Other NIR instruments

IAC programs on high spatial resolution techniques and atmospheric optics

Contact

Database (internal)

 

FRIDA's scientific case is very broad: it ranges from solar system bodies to high redshift systems, including close binary systems, young stellar objects, circumstelar phenomena in advanced stages of stellar evolution and active galactic nuclei.

A number of scientific challenges for FRIDA are identified here:



High redshift at kpc scales with FRIDA


- The panoramic view:
 FRIDA => Diffraction limit imaging in JHK on 40” x 40“ FoV

- Microscopic view:
 FRIDA => 2D spec with < 100 mas resolution and a suite of spectral resolutions:

R= 75 km/s  => galaxy dynamics => Mass
R~ 200 km/s (JHK at once)  => Gas diagnosis => galaxy classification

The challenge for AO-assisted instrumentation at high redshift is to get targets with a bright star next to it. The figure below shows examples of  B-dropouts, from the HUDF, corresponding to  the redshift range 3.5 < z < 4.7 (Beckwith et al. 2006, AJ 132) . Object sizes are typically less than 0.5 arcsec and thus FRIDA spatial scales are ideal for their detailed spectroscopic study. Unfortunatly, these objects are difficult to observe with AO instruments due to the lack of a relatively bright star  next to it. Thus, we call the attention of the GTC community on the planning of current or future  surveys, we  encourage survey teams looking for possibilities to explore fields with a relatively bright star, V< 16, in it so that  potential targets for follow up 2D spectroscopy with FRIDA become possible!


Each image covers 1.9 x 1.9 arcsec^2 (13 x 13 kpc at z ~ 4). The FoV of FRIDA at its highest resolution mode is about half of that. The sizes of these objects are typically < 0.5 arcsec, thus FRIDA spatial scales are ideal for their detailed spectroscopic study.


FRIDA and the nearest Universe


- The panoramic view:
 FRIDA => Diffraction limit imaging in JHK on 40” x 40“ FoV

- The microscopic view:
 FRIDA => 2D spec with 40-100 mas resolution and spectral resolution R= 75 km/s

FRIDA spatial resolutions allow us to study galaxies in the near Universe with unprecedented detail:

FWHM ~ 100 mas => ~ 150 pc @  z=0.05
FWHM ~ 100 mas => ~ 13 pc @ Virgo => galaxies across the Hubble sequence
FWHM ~  45 mas => ~  0.7 pc @  M82 => the nearest starburst
FWHM ~  45 mas => ~  0.2 pc @  M31 => the nearest spiral

As an example, the figure below show adaptive optics VLT images, in the 1 to 2.5 um range, of the central parsecs of some of the nearest galaxies in Southern Hemisphere. These galaxies are part of a international observational program, PARSEC, with VLT and Keck aimed at uncovering the central few parsecs of the brightest and closest galaxies in the local Universe.


In each panel, quoted values at the centre of the figure indicate the spatial resolution in physical scales (FWHM < 0.1 arcsec), and represent an upper limit to the nucleus size in each galaxy, In two cases so far, the nucleus has been resolved in the IR: Circinus (FWHM ~ 2 pc, at 2µm, Prieto et al. 2004, and at 10 µm, Tristram et al. 2007), and    NGC 1068 (~2 x1 pc  at 10 µm , Jaffe et al. 2004 and at 2 µm, Weigelt et al. 2004.)

... and even closer: resolving stars in Andromeda

Andromeda, the nearest spiral galaxy to Earth, will be seen with FRIDA down to scales of 1/6 of pc at 2 µm. At these esolutions, it shall be possible to resolve stars down to the tip of the RGB and AGB stars, which in Andromeda are brigther than K<18 mag. Moreover, RGB stars span a wide range of ages, 106 to 109 yr, their detection across Andromeda shall make them suitable candles for:

=> tracing the different stellar population in the halo, disk, bulge, arms,  from which ages could be estimated and thus, clues on Andromeda history formation be derived.

=> tracing chemical enrichment across the galaxy.

=> kinematics of individual RGB stars => accurate determination of galaxy potential.



Spitzer images of Andromeda -above: NASA/JPL/Caltech/P.Barmby, Harward-Smithsonian CfA, PR 2006 - reveal a large concentration of dust across the disk. FRIDA will be able to see through this dust and explore tiny regions of the galaxy with a resolution  25 times larger than that of Spitzer.
 


This is a synthetic color-magnitude diagram (CMD) generated for a stellar population located at M31's distance (Marin-Franch, 2007). It can be seen that the tip of the RGB is brighter then K=18



FRIDA in our galaxy (sub-parsec scales)

- The panoramic view:
FRIDA => Diffraction limit imaging in JHK on 40” x 40“ FoV


- The microscopic view:
FRIDA => 2D spec with 45 mas resolution and spectral resolution down to R= 10 km / s

FRIDA  will allow us both, parsec-scale  studies of  a large number of galactic sources  (HII regions, HH objects, binaries, planetary nebulae, stellar disks …) but also accurate spectral diagnosis of many of these sources (stellar atmospheres, metalicities, ages) thanks to its very high  spectral resolution.

The figure below illustrates the  case of ultra compact HII regions. These are very dusty regions where massive stars come to light. The new born stars  are embedded in their parental cloud and therefore the mechanisms by which star formation sparks can only be explored in the IR.



The left panel shows an optical image of the compact HII G61.48+0.09, the right panel shows the same region observed  in the IR with the AO system ALPHA at the Calar Alto observatory. The IR image  uncovers  a large number of hidden stars, among which  the brightest,  a K=9 mag star is thought to be the lionizing source of the HII region. FRIDA will provide similar images but with the add-on of a very  accurate spectral characterization of the source with resolutions of 10 km/s (from E. Puga et al. 2004 A&A 425). 


Top


FRIDA Project  |  Instrument Overview | Science Drivers  |  IAC Contribution  |  IAC Project Team  |  Sky Coverage

Other Instruments | IAC Programs | Contact | Database

© Page maintained by the FRIDA group at the IAC s