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Slide 11
Notes:
The catalogue entries in the measurement window provide links to other relevant web pages where available. For the MERLIN+VLA source catalogue, you can view plates from the paper. The radio contours are at (1, 2, 3..)x10 microJy in all panes, superimposed on HST or CFHT images.
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Slide 12
Notes:
Aladin can also be used to make contours.
Expand the folder RadOptCut36 and display Rad36. Zoom in on the brightest source. Use the histogram to reduce the radio noise background. Keep the pop-up colour map fixer window open and click on the Contour button. Use the histogram levels as a guide to select the contour levels and select 'current zoom only' for speed. The contours become a plane in the stack. They can be activated/hidden like a catalogue and will correctly overlay any image chosen from a lower plane.
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Slide 13
Notes:
Display Opt 36. Leave the radio contours on. The bright optical source is over an arcsec away, much further than the astrometry errors in these images or in the radio, x-ray and redshift (Keck) catalogues. The cyan optical photometry catalogue source shown just north of the radio source is actually associated with the southerly optical source.
This radio source, J123651+621221, does have an x-ray counterpart and the ISO source to the left is probably associated. There is in fact no HST counterpart detected down to 28 mag apart from a faint NICMOS (very red) source, suggesting a redshift of 2 - 3. Despite this, the absence of a compact radio core and likely ISO detection suggest it is a dust-obscured starburst rather than an AGN.
Mark the source position using the Tag button.
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Slide 14
Notes:
In order to visualise x-ray emissioin associated with these sources it is necessary to go back to the lowest set of images smoothed to the CHANDRA resolution. Turn off the catalogues so the tags can be seen more easily and display the RGB image.
Use the Magnifying glass to inspect the sources. J123652+621444 has relatively bright x-ray emission as well as radio and optical, consistent with being an AGN.
Note the bars at the top of the zoom window show the relative intensities of the pixel at the mouse position in the main view window. The intensity values for each component (radio, optical, x-ray) are on a scale from 1 - 255 normalised for each image separately.
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Slide 15
Notes:
Inspect J123651+621030. This starburst galaxy has significant x-ray emission but the radio and optical emission is relatively brighter.
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Slide 16
Notes:
You can also zoom directly into the source. The radio contours from the high-resolution cutout are shown here on top of a zoom into the position of J123651+621221. There is some x-ray emission although a careful adjustment of the colour map histogram is needed to confirm it is associated with the nore northerly, radio, source rather than the optical (false colour green) source.
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Slide 17
Notes:
Make sure all the catalogues are turned on and zoom out. Turn on the x-ray counts and radio flux filters. These are shown over the smoothed RGB image; the filter symbols may be easier to see over the Opt0.492 image (HST image smoothed to CHANDRA resolution) depending on your screen. The filters are described inside the scripts. Circle size is proportional to source brightness: the red circles show radio detections <100 microJy, the orange circles show brighter radio sources. The blue circles show x-ray detections <80 counts; the cyan circles show brighter x-ray sources.
At first glance there are many radio-x-ray associations, including the fainter sources. This suggests that there is a population of faint starburst galaxies which at present we detect in radio and x-ray out to an average redshift of around 1. However close inspection shows the radio and x-ray emission is often offset by a few hundred milliarcsec (less than the average 1 - 2 arcsec size of these radio sources) and the radio and x-ray flux densities are not well correlated. This suggests that the emission is produced at least partly by separate mechanisms within the same host galaxy, e.g. an embedded AGN in a starburst galaxy.
The radio source catalogue is complete down to 7 sigma (27 - 40 microJy) but there is a statistically significant excess of 3 - 7 sigma radio emission associated with optical sources of I mag 25 or brighter. The next step will be to see if a similar correlation is found with CHANDRA sources.
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Slide 18
Notes:
The size of the green circles is proportional to redshift and it can be seen that most radio sources are associated with relatively low redshift (around 1) galaxies. Only a very few stand out as lying in large green circles. Click on 12:36:42+62:3:31 (or enter the coordinates in the coordinate boc to send the reticule there) and see from the radio catalogue entry that this is relatively bright ( 427 microJy). Scrolling the measurement window shows it is an AGN at a redshift of 4.4.
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Slide 19
Notes:
Enter 12:37:05+62:15:55 in the coordinate windiw and press return to send the reticule here, and zoom in on this region which contains three x-ray sources. Note that the original resolution of the CHANDRA data is several times coarser than the MERLIN+VLA data. None of the x-ray sources have catalogued radio counterparts but they appear to have faint associated radio emission. As mentioned, examining the whole HFF/HDF(N) region may reveal a statistically significant excess of radio emission at the position of x-ray sources or v.v.
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Slide 20
Notes:
Zoom out again. Use the coordinate window to send the reticule to 12:36:46+62:14:48 and zoom in. There are two unclassified radio sources. Select the catalogue entries associated with the right-hand source.
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Slide 21
Notes:
You can also add the catalogue entries associated with the left hand source, without including the un-associated optical source, by using shift-click on the desired catalogue sources.
Use the SED button and toggle the x-axis button in the SED window to show a log scale.
You can click on the mark button to label the corresponding SED point and the source marker in the image in the view window will blink. This makes it easy to see that the brighter radio point is the rightmost source, and the fainter point is more likely to be associated with the ISO source to the left.
You can also remove points from the SED display using the show button.
So maybe using x-ray and other information or loading the appropriate cutouts (22) and inspecting the optical and radio morphologies you have a theory as to the nature of these sources?
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Slide 1
This demonstration illustrates some research possibilities within the capabilities of the prototype Aladin + SED tool released in January 2003.
These images provide the first opportunity to compare directly the astrometrically aligned CHANDRA, HST and MERLIN+VLA data over the whole region of overlap (>8' square). The examples here include:
1) Source classification using multi-wavelength flux density and morphology comparisons
2) The correlations between flux density and redshift
3) The correlations between radio and x-ray emission, especially for sources too radio-faint to include in the catalogues of secure detections.
Note that the discussion in this demonstration is not definative - please refer to the original papers (or do further analysis yourself) before drawing any scientific conclusions!
Also note that in some cases the zoom or colour table was adjusted to get a good screen-shot so your Aladin may not show exactly the same.
This demonstration uses scripts to load data, catalogues and filters. Read the comments in hdfn.ajs to see how to set this up. For the suggested directory structure run this by typing:
./Aladin < HDFNscripts/hdfn.ajs
In these screenshots, the coral box summarises what is in the main view window. The yellow boxes with red numbers give actions and the order to perform them, the unnumbered boxes are descriptive.
The plane stack is loaded from the bottom up but you can change the order by dragging the icons.
The FITS images are loaded from the Jodrell Bank web server as the radio and optical images have been aligned to the ICRF and either smoothed to the CHANDRA resolution (0".492 pixels) or made into cutouts at 0".0625 resolution. See HDF North Notes and links for more details. The catalogues are loaded from Vizier.
Filters:
These filters are created in a hidden state. To see the effect of a filter:
1) Place it higher in the stack than any catalogues you want it to select from. Note that filters operate on any and every catalogue lower in the stack, on the first (if any) column with a label or UCD corresponding to a column label or UCD specified in the filter.
2) Activate the catalogues so the positions of the catalogue sources are displayed.
3) Activate the filter and the catalogue markers will be turned off and replaced by the symbol specified in the filter if any catalogue entries satisfy the criteria in the filter.
Make the plane stack more managable by using the 'Eye' pull-down menu to create folders. Drag them into place above each set of images (above each RGB image and above the top image); drag the images into the folders; use the Properties button to rename the folder and then collapse folders you are not using.
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Slide 4
Open the lowest folder and display the smoothed RGB image, and adjust the colour map using the Histogram button. Note that each component image look-up table is normalised, with the brightest pixels having value 255; this is particularly useful for images like these containing many faint sources only. The radio (red) histogram shows an almost Gaussian noise distribution with just a small excess of significant sources. The optical (green) histogram shows a peak in the distribution for very faint sources. The sawtooth distribution of the x-ray (blue) histogram is due to the nature of the CHANDRA detectors.
Enter the coordinates 12:36:44+62:11:33 in the Coordinate window and press return. The reticule (mauve +) moves to this position. Click on the Magnifying Glass and move the cursor to the source near the reticule, it appears enlarged in the Zoom window.
The core is white, showing it is bright at all wavelengths. Radio jets (false colour red) extend north and south. This is an FR1 type AGN, J123644+621133.
There are three ways to zoom:
1) Using the Zoom pull-down menu (zooms in or out on the current centre; the field of view can be changed using the box in the Zoom window);
2) Using the Zoom button to zoom about a point chosen with the mouse;
3) Using the Magnifying Glass button.
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Slide 5
Collapse the bottom folder. Expand the next one up (RadOptCut20) and display Opt20_0.0625, a high-resolution HST cutout image. Use the Zoom button to zoom out to x1/4 (note this is still smaller than the previous smoothed resolution field of view).
Use the left mouse button to select the catalogue points near the brightest source and the entries are displayed in the measurement window at the bottom. Note that the entry for the optical photometry catalogue (cyan symbols) is offset, but if you hover the mouse over catalogue entries you find that it and the radio (red) and redshift (pink) catalogues all contain I mag. measurements close to 18.5 and there are no other bright sources nearby in the optical image.
Look at the whole view window - the cyan + catalogue sources (optical photometry from J/AJ/119/257) are systematically offset a few arcsec north of other symbols. The radio and x-ray (red and gold) sources can be assumed to have the best astrometry (see links in slide 2.).
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Slide 6
The leftmost column in each catalogue entry in the measurement window contains a link to Vizier. This should pop up in a browser window but you may need to have a browser already running or, as with other Aladin windows, it may create it in a closed state on your desktop or as an icon, if you have already closed a similar window.
You can then follow the links in the browser to see what information the original paper provides. In this case we select the optical photometry catalogue (cyan symbols) and the corresponding paper by Vanden Berk et al. describes how the data were taken using the relatively small McDonald telescope and a few arcsec uncertainty is not surprising.
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Slide 7
Select the corresponding RGB image for cutout 20 and zoom in on the brightest source, J123652+621444. If you have not already selected the corresponding catalogue entries, use the mouse in the view window to display these in the measurement window (including the cyan optical photometry point offset a few arcsec to the north). Then click on the SED button which will pop up a window which plots the radio and optical points. The optical photometry measurements (in magnitudes) have been converted to Jy. The x-ray data are not shown as counts cannot yet be converted.
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Slide 8
J123652+621444 has
1) radio flux density > 100 microJy (from catalogue entry shown in measurement window)
2) a steep radio-optical spectrum (SED tool)
3) a compact radio core inside extended optical emission.
This is typical of weak AGN in the HFF/HDF(N) - two thirds of radio sources brighter than 100 microJy are AGN. Although many are at redshifts around 0.3 - 1.3 , some are at redshifts of 2 3 or 4.
Mark the source position using the Tag button - as long as the corresponding plane is activated the tag position will be marked on any image lower in the stack.
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Slide 9
Collapse the folder for RadOptCut20 and expand the RadOptCut52 folder and display the RGB image.
The default display of a new image is the inner 512x512 pixels and these are 1024x1024 images. The brightest source in this cutout is just outside the inner region so use the box in the Zoom window to find it, and then use the Zoom button and the mouse to zoom in.
As before, select the catalogue entries near the source and plot the SED. The ISO catalogue source is probably associated as the ISO errors can be 3- 9 arcsec. This source, J123651+621030, has bright IR emission and a radio flux density <100 microJy.
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Slide 10
Zooming in on J123651+621030 shows that it has a larger (false colour) white core than the previous source, and there is both radio (red) and optical (green) extended emission. These diagnostics -
1) radio flux density <100 microJy
2) bright IR emission
3) radio emission extended over a couple of arcsec
- are typical of starburst galaxies in the HFF/HDF(N). Over two thirds of the identified galaxies fainter than 100 microJy are starbursts.
Most of these are at redshifts between 0.3 - 1.3.
