As I have many colour images in my notes which will not print out as colour images on our printer, I have the various Figures collected here for anyone to browse through.
The previous page with ps and jpg images has been removed and the name now points to this page, since it is easier for people to deal with gif and jpg files instead of ps files.
Some of these images are taken from other sources. These are all properly referenced in my notes, but I do not have the references here. The Figures are listed below in (I hope) the same order as in the lecture notes.
After the images from the notes, I give a fair number of additional images that I picked up after making the notes. Various of these were used in the class.
On this page all images are in GIF form unless noted as JPG or TIFF form.
All sky images, which were created by Axel Mellinger, who is a very accomplished astrophotographer, can be seen in the following two links: All sky panorama in galactic coordinates (JPG) Same thing in equatorial coordinates (JPG), with the northern hemisphere at left and the southern hemisphere at right. The center of each circle is one of the sky poles, and the border of each circle is sky equator. This is similar to the projection used for many posters of the constellations. Annotated version of the equatorial image (JPEG) Annotated version of the equatorial image (TIFF)Here is another annotated version of the equatorial image; this is what is sent by Sky and Telescope when you purchase the poster.
See below for the COBE and 2MASS all-sky panorama images at longer wavelengths.
Introduction Section: Lund Observatory all sky picture Milky Way Panorama (JPG) Full size Milky Way Panorama (JPG) Milky Way Panorama Overlay (JPG) COBE NIR sky image COBE FIR sky image (See below for better versions of these last two Figures, released in May of 2000.) ISM Spectrum
Ionized Gas: HII Regions and Planetary Nebulae Rosette nebula image M4-18 optical spectrum Oxygen III forbidden line energy level diagram Electron temperatures in different HII region models Ionizing photon fluxes in HII region models Electron density in HII region models Model radio spectrum Normal composition HII region model spectrum Normal composition PN model spectrum Dusty HII region model spectrum Observed spectrum of NGC 7027 Infrared spectrum of the Orion Nebula
Molecular Line Emission: HVC Map In HI (JPEG) CO molecule rotational energy levels CO molecules rotational/vibrational energy levels CO map of the galactic plane CO map of the inner galaxy CO map of NGC 891 Map of nearby molecular clouds FCRAO CO Map CGPS Figure 1 (JPEG) CGPS Figure 2 (JPEG) CGPS Figure 3 (JPEG) Energy level diagram for OH Energy level diagram for NH3 (JPEG)
Original Canadian Galactic Plane Survey Images (all TIFF images): 74 cm mosaic from about 125 to 145 degrees longitude CO emission from local arm velocities CO emission from Persues Arm velocities HI emission from local arm velocities HI emission from Persues Arm velocities 12 Micron Map of Region 25 Micron Map of Region 60 Micron Map of Region 100 Micron Map of Region
Columbia CO survey colour poster (JPG) See this link for the original images.
Supernova Remnants: Example SN spectra Similarity solution plot Superbubble in the LMC (JPG) Crab nebula in x-rays (JPG) Crab nebula in the optical (JPG) Crab nebula in the infrared (GIF) Crab nebula at radio wavelengths (GIF) Cas A in x-rays (JPG) Cas A in the optical (JPG) Cas A in the infrared (JPG) Cas A at radio wavelengths (JPG) N132D in x-rays (JPG) N132D in the optical (JPG) N132D at radio wavelengths (JPG) Cygnus loop in x-rays Optical image of the Cygnus loop Radio image of the Cygnus loop Infrared image of the Cygnus loop and surroundings Hb9 x-ray image Hb9 radio image The Barnard 68 Dark CLoud (JPEG)
Dust in the ISM: The standard extinction curve Mie theory results 1 Mie theory results 2 Mie theory results 3a Mie theory results 3b Forsterite grain m values Mie theory results 3c Quantum heating plot 1 Quantum heating plot 2 Quantum heating plot 3 Red Rectangle spectrum Red Rectangle image
Giant Molecular Clouds: Orion nebula region in CO High resolution CO map of the Orion Nebula Structures in the Orion region Infrared map of the Orion region A colour photographic image of the Orion region (JPG) Optical image of the Orion Nebula Another optical image of the Orion region Closer view of the Orion Nebula HST image of the Orion Nebula Optical and radio maps of the Orion Nebula HST Image of the Trapezium (1) HST image of the Trapezium (2) 2MASS K-band image of the Trapezium region BN/KL region at 20 microns Identification of objects in the BN/KL nebula Explosive activity in the BN/KL region Explosive activity in the BN/KL region (2) (JPEG)
Star Formation: Isothermal Collapse Similarity Solution 1 Isothermal Collapse Similarity Solution 2 Isothermal Collapse Similarity Solution 3 Optical spectra of typical T Tauri stars Optical spectra of T Tauri stars 2 (JPEG) Extreme cases of line emission from T Tauri stars (JPEG) Shorter wavelength optical spectra of T Tauri stars 1 (JPEG) Shorter wavelength optical spectra of T Tauri stars 2 (JPEG) Herbig Ae/Be Star HR Diagram Variability of BF Ori Spectral energy distributions of two Herbig Ae/Be stars ISO infrared spectra of two Herbig Ae/Be stars Observations of a disk around AB Aur Light curves of FU Ori variables (JPEG) Partial optical spectra of FU Ori stars (JPEG) The spectral energy distribution of FU Ori (JPEG) NIR spectra of two FU Ori stars (JPEG) Molecular lines observed towards NGC 2023 ISO Observations of RAFGL 7009S ISO Observations of L1551 IRS5 ISO Observations of NGC 7358 IRS9 ISO Observations of T Tauri Wings of the molecular lines from NGC 2023 (JPEG) Map of the high-speed CO emission in NGC 2023 MM1 Molecular outflow from IRAS 20126+4104 Molecular outflows from low mass YSOs (1) Molecular outflows from low mass YSOs (2) HST image of HH1/2 (JPEG) HST image of HH30 (JPEG) HST image of HH47 (JPEG) VLT image of HH34 (JPEG) HST NICMOS images of YSO disks (JPEG) HST images of YSO disks (JPEG) HST images of YSO disks (JPEG) VLT image of L1551 at 7 mm An optical image of the LMC (JPG) An optical image of M33 (JPEG) The NGC604 giant star formation region is the red knot at upper left. This picture is by David Malin, from original images made on the Isaac Newton telescope in the Canary Islands. Optical/X-ray image of 30 Dor Wide field optical image of 30 Dor (JPEG) HST view of R136a HST image of NGC 604 in M33 (JPEG) VLT image of NGC 3603 (JPEG) HST image of NGC 4314 (JPEG) Optical image of NGC 1569 Optical image of NGC 4214 (jpeg) This is a nearby galaxy with active star formation. See the page here for more information. Added images: (not in notes at present) NGC 891 optical image NGC 891 near-infrared image (JPG) Three colour composite of the Rosette Nebula (jpeg). In this image the balmer alpha line image is coded in red, sulfur emission (likely from the S+ 6717/6731 forbidden lines) is coded in blue, and oxygen emission (likely from the O++ 4959/5007 lines) is coded in green. One sees that the blue/green emission is from the inner parts of the nebula and that plain H alpha dominates the outer regions. One also sees some dust lanes in the nebula. The image was the APOD for 11 January 2000, courtesy of T. A. Rector, B. Wolpa, and M. Hanna. Optical Spectrum of M1-6, showing some of the forbidden lines. The OIII lines at 4959/5007 Angstroms are analogous to the NII lines at 6548/6583 Angstroms; they are both from the p2 electronic configuration as discussed in the notes. The SII lines at 6717/6731 Angstroms are from the p3 electronic configuration. The analogous OII lines are in the blue part of the optical spectrum and so are not shown in this plot. Hydrogen energy level diagram (JPEG). Illustration of two-photon emission (JPEG). Helium I energy level diagram. Oxygen II forbidden line energy level diagram. Model Radio Image of a SNR This is a model image using the similarity solution for the adiabatic phase to predict the radio surface brightenss of the SNR. Due to the higher density and lower temperature on the outside of the remnant, it looks very much like a thin shell seen in projection. FUSE Observation of Coronal Gas The Far-Ultraviolet Spectral Explorer satellite (FUSE) was recently launched and is providing spectra of objects in the short wavelength ultraviolet, from the Lyman Alpha line down to the Lyman limit. This image shows the result of one such spectrum, with many ISM absorption lines marked. The spectrum includes lines of molecular hydrogen in the cold ISM, the Lyman beta line at 1025 Angstroms, some lines of atomic species of low ionization from the warm phase of the ISM, and a line of highly ionized oxygen (O VI, 1031.9 Angstroms) from the very hot phase of the ISM. FUSE Model of Coronal Gas (JPEG) This picture shows a model of the far-UV emission from the galactic disk, along with the diffuse bubble-like structures from the hot phase of the ISM. This model is based upon some results of the FUSE satellite (see the spectrum above) along with SNR evolution models. Chimney in the ISM from the CGPS (JPEG) The CGPS has found some "chimneys" such as shown here, places where the ISM gas is "blown out" allowing material to move off the plane up to high galactic latitudes. This supports the general picture of the multi-phase ISM. An X-ray image of the Orion Nebula Region (JPEG) The young stars in Orion tend to have x-ray emission, as is shown in this x-ray image of the Trapezium and surrounding region by the Chandra X-ray Satellite. The field of view is about 19 arc-minutes square, or 10 light years across at a distance of 1800 light years. The Trapezium stars are at the center of the image. A 330 MHz Image of the Galactic Center (JPEG) This image, from Kassim, Briggs, Imamura, Lazio, LaRosa, and Hyman (2000; Astron.J., vol. 119, 207-240), shows the region of the Galactic Center in a low-frequency radio map 4 degrees by 4 degrees in size, and with angular resolution 43 arc-seconds. Many of the interesting structures are shown. See their WWW paper for more details. HST image of the NGC1999 Globule (JPEG) Image of the Rho Oph GMC region (JPEG) Schematic of local ISM structure Artistic view of the local ISM structure Here is another diagram showing the structure of the local ISM, due to Linda Huff and Priscilla Frisch. It shows the very local structure. The local ISM is strongly influenced by the Scorpio-Centaurus association, which is the nearest site of recent formation of relatively massive stars (the nearest current site of massive star formation is the Orion Nebula). From this figure, it seems that Alpha Centauri, Sirius, and Procyon are all in the local hot bubble and the Sun is in a filament of denser gas intruding into the local bubble. Altair marks the general direction of the Scorpio-Centaurus association. Wide-field image of the Orion region (JPEG) Optical image of NGC 1999 and area (JPEG) Near-infrared image of NGC 2024 and area (JPEG) Image of the HH111 Jet (JPEG) Deep NIR image of the Trapezium region This image was taken at the UKIRT with a new NIR camera named UFTI; the three colours correspond to three filters in the 1 to 1.5 micron range (I do not know the details....) and the very red objects are low mass stars, brown dwarf stars, or free floating planets. The planets and brown dwarfs are expected to be brighter in the IR when they are young, as is the case here. Dr. P. Roche and Dr. P. Lucas took these images; their press release states that they have identified 13 free planets and about 100 brown dwarf stars in the field. Various of these have been confirmed -- to some degree -- by spectroscopy. Some sample galaxy spectra (JPEG) This is from a review paper on "Star Formation in Galaxies Along the Hubble Sequence" by Robert C. Kennicutt Jr. (Ann.Rev.Astron.Asph., 36, 189-231, 1998). The lowwer two spectra, of later type galaxies, show signs of strong star formation in the emission lines. NGC 4449 has the [OIII] 5007/4959 angstrom lines about as strong as H-alpha, which indicates very hot stars are being formed. The strong line at the blue end of the spectrum is [OII] 3727. Wide-field Image of the LMC and the SMC The LMC is at left and the SMC is at right. This was taken by W. Keel of the University of Alabama at Tuscaloosa on the Cerro Tololo telescope. Image of M82 (JPEG) This is a Subaru composite image of M82, which codes the B and V filter images in blue and green along with the H-alpha image in red. The line emission is from a region out of the plane. Image of M82 (JPEG) This is a similar image contrasting a continuum image of M82 (white) with the 5007 [OIII] image of the same region (yellow). This is work by Gail Conway. Another schematic of the local ISM Image of NGC1850 (JPEG) This is a young globular cluster in the LMC, estimated to be about 50 million years old. It is (probably) inside N57D, a SNR in the LMC. Right behind the main cluster is another small cluster of even younger stars, some 4 million years old. This is a B/V/H-alpha composite showing a 300 by 300 light-year field. HST image of NGC1850 (JPEG) This is a close-up of the NGC1850 globular cluster. It is a false-colour image, probably in the UVI filters. Multi-wavelength picture of SNR E0102-72 This is a picture from the Chandra x-ray telescope group (NASA/CXC/SAO) showing a SNR in the LMC in three different bands as a false-colour image. A radio map is coded in red, and optical map is coded in green, and the Chandra x-ray map is coded in blue. One sees a nice stratification of the gas here. The radio emission is due to the synchrotron process and so it marks areas with magnetic fields and energetic electrons. The x-ray emission is straight thermal emission from the coronal gas. The optical emission is from embedded cooler clumps where some recombination is occuring, resulting in oxygen emission lines. X-ray Image of M82 This newly released x-ray image of M82 from the Chandra satellite shows why the H-alpha and O++ emission from M82 has the form that is shown in the previous images. Here in the x-ray image one sees that something -- most likely multiple supernovae -- has formed a very large double-bubble structure out of the plane of the galaxy on either side. Some individual SNRs are probably seen in the center of this image. None of this structure can be seen in the optical continuum images of M82, since the extinction to the core starburst region is quite large. COBE NIR sky image This is ths COBE NIR data on an all-sky colour coded map (red for L, green for K, blue for J) which has been re-proceesed to get higher sky resolution. See the source page http://www.astro.ucla.edu/~wright/CIBR/images.html which gives more details of the processing. The image has 3 panels: the original data, the data corrected for zodiacal light, and then the assumed emission with the galactic foreground emission subtracted. The latter step cannot work properly for the brighter parts which are therefore excluded. The zodiacal light component is the diffuse blue component crossing the galactic center at a sharp angle (roughly 70 degrees up from the right side) and then following the upper right/lower left edges of the image. COBE FIR sky image This is the reprocessed FIR image, similar to the last image, but using 240, 100, and 60 microns for the colour codings. COBE NIR sky image The same zodiacal light subtracted COBE NIR image as above, but with the contrast enhanced. Illustration of a warped spiral galaxy disk This image, from the HST Heritage Team and Chris Conselice of the Univeristy of Wisconsin, shows a spiral galaxy (ESO 510-13) with a large warp in the disk. ESO 510-13 is thought to be about 46 Mpc away, and is about 30 kpc in diameter. Its radial velocity is 3455 km/s. Note the promient bulge in the galaxy. ESO 510-13 is found in the southern constellation of Hydra, roughly 13 degrees south of Spica. Another picture of this galaxy, from the VLT, is shown here. If you want a large jpeg version of the HST picture, it is found at this link. H Alpha mosaic of the southern sky This is from the Southern H-Alpha Sky Survey Atlas project, which has mapped the southern sky in the H-alpha line at about 0.8 arc-second resolution. Any stars seen in the images have been removed to produce a picture of the diffuse ISM in H-alpha. The unit "Rayleigh" is defined as 1 million/(4*Pi) photons per square cm per second per steradian. If I have done the conversion properly, 1 R is equivalent to a sky brightness of 5.65981e-21 W per meter squared per square arc-second at the H-alpha wavelength. The conversion factor is inversely proportional to wavelength. If you compare this with Axel Mellinger's all-sky panorama give above, you will see that some of the brighter structures are seen in both pictures. In particular the Orion complex, the Gumm nebula, and the two Magellanic Clouds are easily seen in both images. H Alpha mosaic of Taurus/Orion/Monoceros region (jpeg) This is from the Virginia Tech Spectral Line Survey, the analogous northern hemisphere H-alpha mapping project. It shows the Monceros/Orion/Taurus region of the sky. The loop at lower left is Barnard's Loop, seen in the optical picture of the Orion region above. Inside the loop are the Orion A/B Clouds. To the upper right is the bubble around lambda Ori. The bright compact nebula in the center-right is the Rosette nebula. The galactic plane runs left to right around where the Rosette nebula is. One sees many loop-type structures in the galactic plane. Image of the M78 Reflection Nebula This picture, due to S. Lee, C. Tinney, and D. Malin of the AAO, shows the M78 reflection nebula, a part of the Orion Nebula complex. Wide-field Image of the Orion Nebula (JPEG) This image is due to Robert Gendler, and it was the Astronomy Picture of the Day for February 13, 2002. This image shows a larger region surrounding the Trapesium, with the intensity scale flattened to allow many structures to be seen. One sees the extended, fainter H-alpha emission as well as the bright core of the nebula and the Trapesium stars. This Figure has been flipped in both x and y to match the other images of the Orion Nebula linked on this page. Colliding Stellar Winds This image is an HST, courtesy of the Hubble Heritage Team, showing the young star ll Ori and the surrounding Orion Nebula. This image has been slightly altered from the original image in that I have flipped axes so that north is up and east is at left as is normal. The star, ll Ori, is a T Tauri star. The Trapesium is located up and left of the star, and the stellar wind from this star is colliding with the outflow of material from the Orion Nebula (just the expansion of the ionized region under its excess pressure compared to the surrounding ISM) to produce the "bow shock" seen around the star just to its left. The image is a false-colour composite of images in three emission line filters and one broader-band filter. This was the picture of the day for March 13, 2002. Colour Image of the Orion Nebula (JPEG) This image by Emmanuel Mallart was the Astronomy Picture of the Day for May 30, 2002. The field of view shows the area of the sky where the top of the Orion A cloud and the west edge of the Orion B cloud are seen in the CO images. Since this is an optical image, one sees the HII regions and dark dust lanes. This image is nice because it is more or less in the proper colours and because it shows the brightness distributions fairly well. The two bright stars near the top of the image are the two left-most belt stars in Orion as seen from the northern hemisphere. Above the Horsehead Nebula is the Flame Nebula, where it appears a relatively massive star is forming. 2MASS all-sky image This is an image created from the 2MASS JHK all-sky survey. It uses the JHK filter results for blue, yellow, and red. One sees the disk and bulge of the Galaxy and the Magellanic Clouds quite readily. This is similar to the COBE NIR all-sky image, but with muchbetter sensitivity. Comparison with the all-sky optical pictures of Alex Mellinger above shows that the the Galaxy looks very different in the NIR. Another interesting indication of the sensitivity of this all-sky image is the size of the LMC compared to what it looks like in Axel Mellinger's all-sky image. This was the APOD for 19 July 2002; credit to J. Carpenter, M. Skrutske, and R. Hurt along with the 2MASS Project. At the above 2MASS link one can get to an alternative version of this picture for the galactic plane (JPEG), which was part of a press release at the AAS meeting in January 2002. The bright points in the image are globular clusters (although IRC+10216 and Eta Carina may show up as individual points). One of these, 47 Tuc, is right beside the SMC as can be seen in the wide-field optical image of W. Keel given above. X-ray Image of NGC 1569 (JPEG) Optical Image of NGC 1569 NGC 1569 is a small galaxy which is just outside the local group. It is 3 times as far away as the Andromeda galaxy. NGC 1569 is a galaxy which is just coming out from a starburst episode. The X-ray picture, which is credited to C. Martin at Caltech, was taken with the Chandra Observatory. Different colours are for different energies of x-rays. The companion picture shows what NGC 1569 looks like (see also the pictures above). NGC 1569 has several extremely large star clusters as a result of the recent starburst activity. More information about NGC 1569 can be found at the following two links: the Local Group Home Page J. Stil's NGC 1569 page Colour Image of NGC 300 H-alpha Image of NGC 300 The above two pictures were taken by M. Schirmer and W. Gieren at the European Southern Observatory. The first picture shows the nearby normal spiral galaxy NGC 300 in colour. This is a later type spiral galaxy because the bulge is small. One sees a number of HII regions marking the spiral arms, in red. These are all large HII regions, prehaps similar to the Rosette Nebula in our Galaxy. The galaxy is 21.9 by 15.5 arc-minutes in size, and for the nominal distance of 2.1 Mpc this corresponds to 13.4 by 9.5 kpc linear size. So this galaxy is smaller than the Galaxy, but is similar to M33 in size and general appearance. (M33 = NGC 598 appears to be about 15% to 20% larger in absolute size, and is probably a bit brighter than NGC 300 in the B band.) The second picture is the H-alpha frame that contributed the red colour to the first picture, wherein you see the many bubble-type structures in the arms of the galaxy. One also sees that deliminating spiral arms is not quite as simple as one might hope. These were the pictures of the day for August 21 and 22, 2002. X-ray/Optical/Radio Composite of the Crab Nebula (JPEG) This picture shows a false-colour composite image of the Crab Nebula with radio emission in red, optical emission in green, and x-ray emission in blue. The x-ray picture is from the Chandra x-ray observatory. So this is a composite image made from three of the four images of the Crab Nebula given in the notes, but the main thing is that they are all to scale so one can see that the x-ray emission region is inside the optical emission region which is inside the radio emission region...although the energy contrast between the radio and optical emission is not as great (in linear terms...) as that between the x-ray and optical emission so the overlap is greater. This image is courtesy J. Hester of Arizona State University and was the APOD for September 20, 2002.
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