Links in normal type are to Aladin screenshots on wiki page http://www.euro-vo.org/twiki/bin/view/Avo/Ngc1333Workflow

• Target HH7-11 (near centre of NGC1333)
• Default search radius unless specified
• Load > Aladin Server Selector Tree

NGC 1333 SFR

• • • • IRAS2 ? Class 0? faint water (known class 0 - ISO - multiple?)
      • SVS13 Class 1
• What about VLA2/MM3? Go back to main Aladin window and select VLA source 2

• • • IDHA tree MERLIN NGC1333
    • Right-click in tree to Collapse All and click on RESHIGH
    • In tree, find region K covers MMS3 and click on K to open

• • • • Use Mglss to see flux density ~0.18 mJy/beam in 65-mas MERLIN beam => Tb > 8000 K > ionised outflow
    • VLA2/MMS3 is precessing micro-jet associated with embedded young probably low-mass binary YSO

NGC 1333 SFR

• • SSA Server for ISO Spectra Archive
  • Right click Make Catalogue Plane
  • For LWS01 spectra of IRAS 4, IRAS 2, SVSS13

• • Zoom in on lower ~5 VLA sources and select catalogue points nearby
  • Working up from bottom, VLA sources are
    • VLA25 - IRAS4 region

• • • VLA4 - SVS13
      • very red optical counterpart **check
      • ISO spectrum

• • • Click on Spectrum to load into SpecView
      • Select All in load window
      • In main SpecView window select DQ All

NGC 1333 SFR

• • Set ALLOWTOPICRENAME = TWikiAdminGroup

NGC 1333 SFR

• • Go back to ISO Spectra Server
    • Load SVS13 into Specview and repeat above stages
      • See no water line around 179 um but CO around 175 um

• • • • Omit opening log file as already open (for Demo, no need to measure as log file already prepared).
    • Repeat for IRAS2, use Cursor menu to close log file.
• Load > MyData

• Load > MyData
  • If data are on local network go to e.g. /local/scratch/NGC1333FITS for MERLIN 6-cm images
  • Use existing description file

• • • Right-click in tree to Collapse All and click on RESHIGH
    • In tree, find region K covers MMS3 and click on K to open
      • Click VLA2/MMS3 in main image, scroll down Server Selector tree to highlighted K tile ICL01818

NGC 1333 SFR

• Target HH7-11 (near centre of NGC1333)

• • POSSII N image 12'.8 x 12'.8

• • Radio
    • J/ApJS/125/427 Rodriguez et al. VLA continuum

• • For LWS01 spectra of IRAS 4, IRAS 2, SVSS13

• • • VLA25 - IRAS4 region
      • no optical counterpart apparent
      • ISO spectrum

• • • VLA4 - SVS13
      • very red optical counterpart **check
      • ISO spectrum

• • • • See broad water line in spectrum around 179 um, CO around 175 um
      • Use curly arrow button to return to full view

• • Go back to ISO Spectra Server
    • Load SVS13 into Specview and repeat above stages

• • • Repeat for IRAS2, use Cursor menu to close log file.

• • VOPlot will appear automatically
    • Functions
      • New Column

• • • • • [60-100] = log(S_100/S_60)
        • [100-170] = log(S_170/S_100)

• • • • Y-axis IRAS4[60-100]
      • X-axis IRAS4[100-170]
      • Plot
      • Check Overlay box

• • • • IRAS4 Class 0 - colours, water
      • IRAS2 ? Class 0? faint water (known class 0 - ISO - multiple?)
      • SVS13 Class 1

• • • VLA2/MMS3 is precessing micro-jet associated with embedded young probably low-mass binary YSO

<!--

• • Set ALLOWTOPICRENAME = TWikiAdminGroup

NGC 1333 SFR

• • Set ALLOWTOPICRENAME = TWikiAdminGroup

NGC 1333 SFR

• • Set ALLOWTOPICRENAME = TWikiAdminGroup

NGC 1333 SFR

• Load MyData
  • If data are on local network go to e.g. /local/scratch/NGC1333FITS to get local tree .aladin_idha for MERLIN 6-cm images
  • Use existing description file

• • • In tree, find region K covers MMS3
      • Open K, click MMS3 in main image, tile needed is ICL01818
    • Load and move catalogues above it in stack

NGC 1333 SFR

• Target HH7-11 (near centre of NGC1333)
  • Radius 10 arcmin at all time; close pop-up windows after use

• Vizier cagtalogues
  • Radio
    • J/ApJS/125/427 Rodriguez et al. VLA continuum

• • • Right-click in filter window for shortcuts * CHANGE to DIY filter png
    • filter NGC1333_VLA.ajs if you want pre-loaded

• • Working up from bottom, VLA sources are

• • • • no optical counterpart apparent
      • ISO spectrum

• • • • optical is foreground star
      • ISO spectrum
    • VLA2 - MM3

• • • VLA4 - SVS13
      • very red optical counterpart **check
      • ISO spectrum

• • • Load into SpecView
      • Select all segments
      • In main SpecView window select DQ All

• • • In tree, find region K covers MMS3
      • Open K, click MMS3 in main image, tile needed is ICL01818
    • Load and move catalogues above it in stack

• • • • Use Mglss to see flux density ~0.18 mJy/beam in 50-mas MERLIN beam => Tb > 8000 K > ionised outflow
      • Molecular detections offset
    • VLA2/MMS3 is precessing micro-jet associated with embedded young probably low-mass binary YSO

NGC 1333 SFR

Demonstrates use of:

• • Radius 10 arcmin at all time; close pop-up windows after use

• Vizier cagtalogues
  • Radio
    • J/ApJS/125/427 Rodriguez et al. VLA continuum

• Main Aladin Filter button
  • Aladin filter to select sources with S_6cm>200 uJy & classified as YSO

• Zoom in
  • Working up from bottom, VLA sources are

• • • (omit the others for simplicity)

• • ISO Spectra Server
  • For LWS01 spectra of IRAS 4, IRAS 2, SVSS13
    • Note red line to show position in main image

• • • • Make colours for each source
        • [60-100] = log(S_100/S_60)
        • [100-170] = log(S_170/S_100)

• • • • Y-axis IRAS4[60-100]
      • X-axis IRAS4[100-170]
      • Plot

• • • • • View menu select Whole Data Range
    • Compare with Pezzuto et al. ISO-LWS two-colour diagram of young stellar objects
      • IRAS4 Class 0 - colours, water

• • • • SVS13 Class 1

• Vizier cagtalogues
  • Radio
    • J/ApJ/463/205 Anglada et al. (CS, NH3 in H2Omaser-selected sources)

• Load MyData
  • If data are on local network go to e.g. /local/scratch/NGC1333FITS to get local tree .aladin_idha for MERLIN 6-cm images
  • Use existing description file

• • • In tree, find region K covers MMS3
      • Open K, click MMS3 in main image, tile needed is ICL01818
    • Load and move catalogues above it in stack
      • Use Hist to set upper flux limit to 3E-4 and Replay autocut

NGC 1333 SFR

• Main Aladin Filter button
  • Aladin filter to select sources with S_6cm>200 uJy & classified as YSO
    • filter NGC1333_VLA.ajs

• Move USNO-B up stack above filter
• Zoom in
  • Working up from bottom, VLA sources are

NGC 1333 SFR

• Target NGC1333
  • Radius 10 arcmin at all time; close pop-up windows after use
• VOTest

• • Select Energy Band 0.1-12 keV and load
• Vizier cagtalogues
  • Radio

• • • • Omit opening log file as already open (actually can use pre-prepared log file for VOPlot)
    • Repeat for IRAS2, use Cursor menu to close log file.
• In main Aladin window

• • NGC1333.logSpecView log file for IRAS4 IRAS2 SVS13.
  • MyData to load log file

• • • Functions
      • New Column
      • Make colours for each source

NGC 1333 SFR

1. VOTest XMM energy band selector
2. Catalogue selection

1. ISO Spectra in SpecView including measurement log
2. Loading measurement log into VOPlot and using functions
3. On-the-fly generation of image tree from user data

• • Optical
    • USNO-B to check for foreground stars
• Main Aladin Filter button

• • • Load pre-defined filter NGC1333_VLA.ajs
• Move USNO-B up stack above filter
• Zoom in

• • MyData to load log file
  • VOPlot
    • Functions

• • • • Make colours for each source
        • [60-100] = log(S_100/S_60)
        • [100-170] = log(S_170/S_100)

NGC 1333 SFR

• • • In tree, find region K covers MMS3
      • Open K, click MMS3 in main image, tile needed is ICL01818
    • Load and move catalogues above it in stack

• • • • Use Mglss to see flux density ~0.18 mJy/beam in 50-mas MERLIN beam => Tb > 8000 K > shock
    • MMS3 is precessing micro-jet associated with embedded young probably high-mass binary YSO

NGC 1333 SFR

• • Optical
    • USNO-B to check for foreground stars
• Main Aladin Filter button

• • • Load pre-defined filter NGC1333_VLA.ajs
• Move USNO-B up stack above filter
• Zoom in

• • • • Select all segments
      • In main SpecView window select DQ All
      • Select Units Jy

• • • • See broad water line in spectrum around 179 um, CO around 175 um
      • Use curly arrow button to return to full view
      • Use Cursor menu to open log file

• • Go back to ISO Spectra Server
    • Load SVS13 into Specview and repeat above stages
      • See no water line around 179 um but CO around 175 um

• • • Repeat for IRAS2, use Cursor menu to close log file.
• In main Aladin window

• • MyData to load log file
  • VOPlot
    • Functions
      • Make colours for each source
        • [60-100] = log(S_100/S_60)
        • [100-170] = log(S_170/S_100)

• • • • Y-axis IRAS4[60-100]
      • X-axis IRAS4[100-170]
      • Plot
      • Check Overlay box
      • Select colours for other sources on axes and plot.
        • View menu select Whole Data Range

• • • • IRAS4 Class 0 - colours, water
      • IRAS2 ? Class 0? faint water (known class 0 - ISO confused?)
      • SVS13 Class 1

• • Radio
    • J/ApJ/463/205 Anglada et al. (CS, NH3 in H2Omaser-selected sources)
    • SSV13 has water maser only, MM3 has all 3 molecules - High mass?

• • Use existing description file

• • • In tree, find region K covers MMS3
      • Open K, click MMS3 in main image, tile needed is ICL01818
    • Load and move catalogues above it in stack
      • Use Hist to set upper flux limit to 2E-4 and Replay autocut
      • Use Mglss to see flux density ~0.18 mJy/beam in 50-mas MERLIN beam => Tb > 8000 K > shock

NGC 1333 SFR

• • Radio
    • J/ApJ/463/205 Anglada et al. (CS, NH3 in H2Omaser-selected sources)
    • SSV13 has water maser only, MM3 has all 3 molecules - High mass?

• • /local/scratch/NGC1333FITS to load MERLIN 6-cm images
  • Use existing description file
    • In tree, find region K covers MMS3

NGC 1333 SFR

<!--

• • Set ALLOWTOPICRENAME = TWikiAdminGroup

Could omit some stages e.g. 7 depending on time/availability of data,

1. Use SpecView to examine spectra for H2O line (Nisini ea 2002, Ceccarelli ea 1999), CO (Caux ea 1999) and to derive colours (Pezzuto ea 2002) using VOPlot

• Class implied by JHK colours
• Nature/class implied by presence/absence in radio, optical, x-ray

• x-ray spectra - if only harder x-rays seen (>~3 keV) implies more obscured so younger. However low-mass stars in accretion stage have x-ray suppressed (Briggs et al. 2004 IAUS219). So weak but hard x-ray implies v. young massive YSO or ~class 1 low-mass c.f. proplyds? Soft x-ray implies T Tauri i.e. low-mass PMS?

• • • accuracy of each diagnostic
    • accuracy of matching objects

1. 1. ISO LWS spectra access
   2. ISO image access

• • Tables not yet in Vizier
    1. XMM Preibisch 2003 A&A 401 543 table only available electronically from ADS 2003A&A...401..543P

1. 1. 1. Getting VOPlot to plot RA from R to L
      2. High-resolution radio data (MERLIN) - being processed

1. 1. XMM spectra (as in Preibisch 2003 A&A 401 543) - may not be suitable, XMM expert consulted
   2. Halpha spectra - probably not available in suitable form for this region.

-- AnitaRichards - 16 Nov 2003

• • Set ALLOWTOPICRENAME = TWikiAdminGroup

NGC 1333 SFR

Could omit some stages e.g. 7 depending on time/availability of data,

• • Set ALLOWTOPICRENAME = TWikiAdminGroup

NGC 1333 SFR

Could omit some stages e.g. 7 depending on time/availability of data,

1. 2MASS catalogue gives JHK mags. Use VOPlot to exclude sources with large flux measurment errors, form and plot J-H and H-K colours.
   • J/ApJS/101/117 UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995) actually gives ready-made colours but that takes the fun away...
2. Export subset catalogue of sources with JHK colours indicative of YSO and plot in Aladin (could use filters to select colours typical of each class, or use 'blink' capability to refer to VOPlot).

• • If L available, better separation but still some ambiguity/contaimination.

1. Load XMM image (and Preibisch 2003 catalogue if available)

1. Load optical image and Halpha if available
2. Make RGB, remove contaminants
   • Radio/X-ray sources with no IR counterpart are probably extra-galactic but radio-only could be v. young (Class 0) - might show up in ISO or in radio spec. line catalogues e.g. masers, CS, thermal CH3OH, check a few.

• • Herbig-Haro objects - ends of jets - so associated with young YSO, but can be spatially separate - don't have x-ray

1. Load ISO image(s) if available, compare with other images using contours if catalogues not available (as noted or via ACE)
2. Load ISO catalogue and use filter to select LWS obs. only

NGC 1333 SFR

• • Getting data from SpecView^? into VOPlot to make colour-colour plot
  • Tables not yet in Vizier
    1. XMM Preibisch 2003 A&A 401 543 table only available electronically from ADS 2003A&A...401..543P

1. 1. 1. Getting VOPlot to plot RA from R to L
      2. High-resolution radio data (MERLIN) - being processed

NGC 1333 SFR

• • Tables not yet in Vizier
    1. XMM Preibisch 2003 A&A 401 543 table only available electronically from ADS 2003A&A...401..543P
    2. VLA Rodriguez et al. 1999 AJ 125 427 tables 1 & 2 1999ApJS..125..427R

• Don't know

NGC 1333 SFR

1. Start with 2MASS K image from SkyView^?
2. 2MASS catalogue gives JHK mags. Use VOPlot to exclude sources with large flux measurment errors, form and plot J-H and H-K colours.

1. Export subset catalogue of sources with JHK colours indicative of YSO and plot in Aladin (could use filters to select colours typical of each class, or use 'blink' capability to refer to VOPlot).

1. Load XMM image (and Preibisch 2003 catalogue if available)
2. Load radio (Rodriguez 1999) catalogue if available.
3. Load optical image and Halpha if available

• • Herbig-Haro objects - ends of jets - so associated with young YSO, but can be spatially separate - don't have x-ray

1. Load ISO image(s) if available, compare with other images using contours if catalogues not available (as noted or via ACE)
2. Load ISO catalogue and use filter to select LWS obs. only

• Class implied by ISO spectra and colours
• Age/mass implied by presence of Halpha, mol. lines
• Age/mass implied by presence/absence of x-ray

NGC 1333 SFR

1. Make RGB, remove contaminants
   • Radio/X-ray sources with no IR counterpart are probably extra-galactic but radio-only could be v. young (Class 0) - might show up in ISO or in radio spec. line catalogues e.g. masers, CS, thermal CH3OH, check a few.
   • Optical-only are probably MS stars, but check for faint x-ray/slight far-IR-submm(how?) redenning indicating PMS low/high mass stars.

1. Load ISO image(s) if available, compare with other images using contours if catalogues not available (as noted or via ACE)
2. Load ISO catalogue and use filter to select LWS obs. only
3. Use SpecView^? to examine spectra for H2O line (Nisini) and to derive colours (Pezzuto) using VOPlot

• Class implied by ISO spectra and colours
• Age/mass implied by presence of Halpha, mol. lines
• Age/mass implied by presence/absence of x-ray

ISSUES

• Already being solved
  1. ISO LWS spectra access
  2. ISO image access