Galactic Scenario for AVO Demo 2004

AVO Solutions

Demo use of ISO and XMM data

ISO Use Cases (images, spectra, catalogues)

XMM Use Cases (full-band and multi-band images)

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Related Pages

Current diagnostics for:

AGE

MASS

Other (not explicitly investigated here)

AVO Solutions

ChamaeleonWorkflow

NGC1333Workflow

GalacticPlane

Background investigations

• OtherRegions&Methods
• Chamaeleon SFR investigated the old way

Here is what was possible at the start of the Demo development, requiring manual access to archive web pages and data downloads. now we can achieve all this in one interface; the user does not need to explcitly explore archive web pages (although the option is still there of course).

Data

New data access features implemented in this Demo include

• Direct access using SIA and SSA to the XMM and ISO archives including multi-energy images and spectra respectively;
• Data trees giving heirachical access (IDHA) to multiple images such as hundreds of high-resolution 'postcards' covering a wide field, or data in different wavebands covering the same field;
• Datacube access to 3D images such as the Canadian Galactic Plane Survey, using IDHA and allowing easy selection by the appropriate 3rd parameter e.g. velocity as well as by position.
• Automatic pop-up of SpecView, VOPlot etc. in response to selection of the relevant type of data.

Demo use of ISO and XMM data

ISO Use Cases (images, spectra, catalogues)

XMM Use Cases (full-band and multi-band images)

Milky Way Star-Forming Regions

Science Drivers

Related Pages

Current diagnostics

• AGE
• MASS
• Environment
• Metallicity

AVO Demo requirements

ISO and XMM data for the Chamaeleon SFR*

• ChamaeleonWorkflow
• Ngc1333Workflow
• GalacticPlane
• OtherRegions&Methods

Data

Applications using these data

ISO use cases

XMM use cases

• More Radio Notes

Flow diagram

• • 2-colour [60-100] v. [100 - 170] Pezzuto et al.'s YSO colour classification

• • See Felli et al. 2000 A&A 362 199 for high glat criteria FELLI et al.'s YSO colour selection

Applications using these data

1. needs diagram or VOTable (loca hand-made?) to define colour regions

• Water and CO lines in ISO LWS spectra

• ISO LWS spectra which show CO lines do not have obvious water

• • Class 0 - water (also see Ceccarelli et al. 1999 A&A 342 L21 and Caux et al. 1999 USIS ESA SP-427 643 - H2O and CO in excitation states detected by LWS probably comes from warm regions close to protostar, distinct from low-energy and maser transitions from high-mass YSO outflows)
  • Class I - no water (upper limit [H2O]<10E-5)

Orion, rho Oph and Corona Australis regions probably not use this time

Workflow

Fig.1: Workflow diagram; sample for NGC 1333.

• left : the ISOCAM image centered on the AeBe star HD 97048 (center of the chamaeleon cloud).

• right : the XMM image with the optical contour overlaid. This optical isocontour are very similar the infrared ones. The largest object in the contours is HD97048 but the XMM image doesn't have any conterpart for this AeBe star. On the other hand, the 2 fainter infrared/optical objects are clearly detected in X-ray. They are T Tauri stars.

These are the cursor-driven measurements obtained to do the 2-colour calculation in case 1. below

• • Differential rotation decays with age and thus does x-ray.

• • An XMM-Newton-based X-ray survey of pre-main sequence stellar emission in the L1551 star-forming complex Favata et al. 2003A&A...403..187F
• Lx/Lbol is x~2.5 lower for low mass stars while they are actively accreting, maybe inner accretion disc field interacts with stellar magnetic field to mess up corona.
• Non-accreters have log(Lx/Lbol) ~-2 - -3 (Briggs et al. 2004 IAUS219 "Stars as Suns" ASP Conf Series XXX)

• Massive YSO - x-ray dominated by stellar magnetic origin. As ages on MS, wind emission dominates.

Preparation for the SIRTF Glimpse

ISO data are available for some regions, see Felli et al. 2002 A&A 392 971 for interpretation of ISOGAL data in Galactic plane.

Use VOPlot to plot ISOGAL data in Galactic coordinates and select regions which overlap with GLIMPSE - all deep South. ESO data?

Look for XMM data.

Radio continuum images e.g NVSS and catalogues from several maser surveys are accessible to Aladdin, the detection/not of excited OH and/or Methanol are SFR indicators and are useful in these very crowded and obscured regions. Need to find an interesting GLIMPSE region in N - maybe W50 or W49.

If the various International Galactic Plane Survey data sets held by CADC (radio continuum, HI, CO, Halpha etc.) become accessible to Aladin these may provide usable spectral data or at least images. However they are mostly at low angular resolution and in many cases the main data are spectral cubes.

• • Galactic Plane: [15]<4.5 [7]-[15]>1.8 [7] < 6 (and K - [7] > 4) (3"-6")
  • See Felli et al. 2000 A&A 362 199 for high glat criteria

• • Becker et al. 1994 ApJS 91 347 5 GHz Galactic Plane survey
  • ISOGAL catalogue is available in Vizier?

1. needs

1. needs

1. table in Vizier could be used for comparison etc.

Workflows for the NGC1333, rho Oph and Corona Australis regions could follow a similar patter with the additional use of NVSS or other radio data for the northern regions, and of optical spectra if available.

ISO spectra (SWS and/or LWS) are available for Orion and NGC 1333. The type for objects with spectra are generally Herbig Ae/Be stars or deeply embedded high mass stars.

XMM images are available for both fields but only Orion also has the point source catalogue released.

ISO data on Orion are available e.g. 2003A&A...406..937B and references therein It has been observed by XMM e.g. 2003IAUS..219E.234B.

• few 10E+4 yr (timescale for each Class depends on mass)

• PMS stars with circumstellar disc

• Low-mass weak-line TTs (?protoplanetary disc? gas-poor?)

• High mass (H) AeBe stars have less IR and X-ray but are very optically bright? Emission lines come from disc? Does this become a Vega-like disc (Scuba etc.)

• Li is the first element to be burnt when a protostar gets hot enough for nulceosynthesis, so indicates start of Class I?
• Halpha indicates accretion, easier to see.

Screenshot for ISO+XMM comparison This image contains:

• left : the ISOCAM image centered on the AeBe star HD 97048 (center of

• right : the XMM image with the optical contour overlaid. This optical

There is no ISO SWS or LWS spectra for the 2 T Tauri stars but the CVF spectra (low resolution, from 3 to 16 microns) is available for the whole field.

This example (found by Alberto Salama) may be use to show the difference between intermediate mass stars (AeBe) and low-mass stars (T Tauri). (LaurentCambresy 23 Oct 2003)

1. using LWS low res Nisini et al. ApJ 2002 574 246

• • Becker et al. 1994 ApJS 91 347 (available?)

• There are ambiguities between the age of a YSO and its mass;
• The metallicity and environmental effects are not systematically understood;
• Few or no investigations have dealt with all available data, but restrict themselves to one or two regions of the e-m spectrum.
• Star-forming regions are often very extended (arcmin, even degrees) with structure on all scales from the whole parent cloud down to individual protoplanets, and very dusty and obscured.
• Hence the properties of a given region can be described accurately in a statistical sense but there are usually many individual objects which are anomalous or unknown.

• Build up list of characteristic properties
  • initially from literature
  • eventually also from from VO investigations
• Establish more comprehensive list of diagnostics to establish the age and mass of YSO and eventually their likely evolution.

We invite members of the SWG or anyone else to add/correct the scientific issues and applications suggested below.

Current diagnostics

AGE

Class 0

• few 10E+4 yr
• YSO has started to form but envelope has bulk of mass
• heating from gravitational collapse
• bulky outflows with non-dissociative shocks
• most energy output as sub-mm/far-IR, thermal
• sometimes proximity to radio-bright UCHII Regions (shock triggers collapse) but don't produce them!

Class I

• 10E+5 - 10E+6 yr
• accretion disk, diffuse environment of sub-stellar mass
• IR peak, non-thermal emission also
• outflow with dissociative shocks
• x-ray flares (stellar origin?)

Class II - >10E+6 yr

• PMS stars with circumstellar disc
• Classical T Tauri stars
• Halpha + IR excess

Class III

• weak-line TTs (?protoplanetary disc? gas-poor?)
• optically bright, IR excess (almost) gone
• x-ray

MASS

More massive protostars evolve faster and have outflows e.g. CO which remain molecular. Lower-mass protostars produce ionised outflows. But molecular v. ionised outflows is implied by the AGE Class 0 - 1 distinction also.

Li and Halpha emission is diagnostic of young low-mass YSO (Halpha indicates accretion).

more information please

Environment might be relevant if we investigate Orion and the effects of the massive hot young Trapezium stars on the Proplyds, compare with quiet low-mass YSO region like Chamaeleon or Taurus.

Metallicity probably no immediate application in the demo.

Applications using these data

ISO

NGC 1333 and Elias 29 etc. in papers

1. using LWS Pezzuto et al. 2002 MNRAS 330 1034
   • 2-colour [60-100] v. [100 - 170]
   • background subtraction not essential (easier processing?)
   • Distinguishes Class 0, I, II
   • could deduce range limits or just plot

1. using LWS low res Nisini et al. ApJ^? 2002 574 246
   • Class 0 - water
   • Class I - no water ([H2O]<10E-5)
   • and other more complex line interpretations

1. using ISOCAM Felli et al. 2002 A&A 392 971 (table in Vizier)
   • [15]<4.5 [7]-[15]>1.8 [7] < 6 (and K - [7] > 4) (3"-6")
   • by comparison with UCHII regions VLA 5 & 8.4 GHz
   • Becker et al. 1994 ApJS^? 91 347 (available?)
   • also Is ISOGAL catalogue available?

Using these methods:

1. needs * LWS spectra, doesn't need calibration * Measure flux density at 3 points, find ratios and plot
   • Ideally spectral tool produces VOTable, so use VOPlot.
   • If Pezzuto table 1 is in Vizier, could overplot?

1. needs
   • LWS spectra and some method for recognising H2O lines...

1. table in Vizier could be used for comparison etc.

XMM

• Low-mass stars have more x-ray? Because they rotate faster?

• L1551 (Taurus) has XMM spectra (and it is a MERLIN detection ;)

• Lx/Lbol is x~2.5 lower for low mass stars while they are actively

• Non-accreters have log(Lx/Lbol) ~-2 - -3

• accretion diagnosed by excess [U-V]
• Mbol needed - check how to get this

Schulz et al. CHANDRA obs of Orion etc.

• Massive YSO - x-ray dominated by stellar magnetic origin. As ages on

• Mag fields anti-correlated with age?

• Are Trapezium stars MS, ZAMS or PMS?

• X-rays from proplyds hard, absorbed and variable - suggesting not due to impact of Trapezium wind, but from small (au-scale/stellar) region.

RADIO

NVSS survey already in Vizier - presence of radio emission detected by NVSS suggests UCHII (if not something quite different - check with catalogue). Check - compact (stellar/coronal) radio probably too faint for NVSS?

NGC1333 archive VLA*** Smith et al. 1999 A&A 349 475 Radio counterparts to X-ray bright YSO. Non-thermal > stellar origin (as distinct from UCHII)

If we use Orion then some proplyds are resolved by MERLIN, could see if radio ones are the same as the x-ray ones.

MERLIN also on NCG1333 but only 1-2 sources.

Could also search for maser catalogues?

Could also use precooked 'local' (VLA etc) archive data or maser spectra but maybe too complicated. Would provide high resolution information (e.g. show several distinct protostars in one site) or clues about size of star (high-vel outflow massive YSO; Keplerian disc gives central mass directly...)

Notes relevant if we use more radio than just NVSS.

to be continued

General waffle - Garching 2002 paper Starforming regions at high resolution - Interferometry and the AVO (Richards et a.)

it might also be interresting to have optical spectra (VLT? NTT?) containing the H-alpha and the LiI lines. These two lines are an age indicator in star forming regions and they may help to build a science case between ISO and XMM.

XMM images are available for both fields but only Orion also has the point source catalogue released.

Milky Way Star-Forming Regions

Science Drivers

General waffle - Garching 2002 paper Starforming regions at high resolution - Interferometry and the AVO (Richards et a.)

Some ideas:

• Classification of compact objects- not well understood for entire regions except in a statistical sense, many tenuous assumptions currently employed... VO uses radio-through-x-ray SEDs and line spectra (high v. low mass cores, nature of circumstellar matter, brown dwarfs v. free-floating planets...)
  • Need example objects which are well known
  • Build up list of characteristic properties from VO images, catalogues, spectra
  • Hence discover hitherto unknown characteristics to classify objects which are e.g. too obscured in the optical, or at an unfavourable angle to detect dust disc, etc. etc.

Data

Priority - ISO and XMM and/or spectra?

ISO data on Orion are available e.g. 2003A&A...406..937B and references therein It has been observed by XMM e.g. 2003IAUS..219E.234B. Also need to check which parts of Orion as it is so huge....

Galactic Scenario for AVO Demo

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