Science Results from the SWIRE study
of the Tadpole Galaxy

Interacting System: UGC 10214 The Tadpole Galaxy Click on this link for the results paper. See the movie here.

Disk of the Tadpole, as seen with HST and Spitzer. Blue is g-band (F475W) from HST-ACS (Tran et al. 2003), green is IRAC-1 (3.6 um) and red is MIPS-1 (24 um)

Graphics

• Jarrett et al. 2005 (science results in pdf)

• Figure 1; Optical-infrared panchromatic view of the Tadpole Galaxy (UGC10214). The center image is a composite combination of eight bands (from blue to red colors): U-band (0.348 um), g'- band (0.485 um), r'-band (0.624 um), i'-band (0.774 um), Spitzer IRAC-1 (3.6 um), IRAC-2 (4.5 um), IRAC-4 (8.0 um) and MIPS-1 (24 um). Maps of the individual bands are shown with side panels. The orientation is such that north is to the left and west to the top of the page. All images are shown with a modified n-sigma log-sqrt stretch described in Jarrett et al. (2002). (email me if you would like a high-resolution version)

• multi-wavelength animation of the Tadpole Galaxy (quicktime movie). Optical to mid-infrared windows spanning massive star formation, old "backbone" stars" and the interstellar medium.

• Figure 2; Spitzer-MIPS 70 um map of the Tadpole Galaxy. The log grey-scale ranges from 0.2 MJy/sr to the peak flux in the disk, ~5 MJy/sr. Overlaid in red are contours of the 24 um map: 0.15 and 0.95 MJy/sr, and in black contours of HI column density: 0.6, 1.2, 2.4, 3.6, 4.8, 5.9 10^20 H atoms cm-2 (Briggs et al. 2001). The equatorial coordinates are in J2000.

• Figure 3; HST and Spitzer views of the Tadpole disk. The grey-scale shows the V-band (F606W) from HST-ACS (Tran et al. 2003) at full spatial resolution. Overlaid are contours of Spitzer 8 um imaging, ranging from 0.3 to 5 MJy/sr in surface brightness. The orientation is standard, E of N.

• Figure 4; Tadpole Galaxy disk. The upper panel shows a 3-color RGB composite of the disk: blue is gband (F475W) from HST-ACS (Tran et al. 2003), green is IRAC-1 (3.6 um) and red is MIPS-1 (24 um). The nucleus (N, yellow arrow) and three IR-bright regions are marked E, W, and S. The x-axis field of view is ~1". The orientation is standard E of N. The middle panel shows the optical-infrared SED of the nucleus, integrated using a 12" aperture. The lower panel shows SEDs for three different bright infrared regions in the disk (see top panel). For comparison, five empirical SED templates normalized to the 2.2 um flux; adapted from Silva et al. 1998) are shown: blue corresponds to an old (dust free) L* galaxy, cyan to an S0 disk; green is an Sa/Sb spiral, magenta is an Sc spiral, and red the integrated light from the dusty starburst M82.

• Figure 5; Optical spectra of the UGC 10214 nucleus (top panel) and tidal tail massive star cluster, J160616.85+552640.6 (bottom panel). Residual telluric absorption bands are labeled A and B, while the 5892 A sodium-D emission line is labeled "n.s.".

• Figure 6; The upper panel shows a 3-color RGB composite of the tail, where blue is g-band (F475W) from the HST-ACS (Tran et al. 2003), green is IRAC-1 (3.6 um) and red is MIPS-1 (24 um). The orientation is standard E of N. The x-axis field of view is ~1". The lower panel shows the optical-infrared SED of the two super star clusters; denoted 1 (brighter 24 um cluster to the west) and 2 (fainter 24 um cluster to the east), integrated using a 12" aperture. See Figure 4 for a description of the overlaid SEDs.

• Figure 7; SEDs of the tidal tail clusters, with the underlying starlight and dust continuum removed from the IRAC 8 um band. This diagram represents optical and infrared light that is in excess to the underlying old stellar population (Fig 3). The dashed line represents the hot dust continuum, stretching from 5.6 to 24 um, and is removed from IRAC-4 (8 um) to create the integrated 7.7 um PAH line emission (see Sec 4.2). See Figure 4 for a description of the overlaid SEDs.

• Figure 8; Mid-infrared colors of the Tadpole Galaxy. The upper two panels show the log [F8um/ F24um] ratio versus 8 um flux density, but with the right panel representing the 7.7 um PAH line (in which starlight and dust continuum is removed from the 8 um channel). The lower two panels show the MIR color versus the IRAC-1 (3.6 um) flux density, which represents the underlying stellar mass distribution. The right panel, as before, represents the 7.7 um PAH line. Filled circles indicate the disk locations, and filled squares the super star clusters in the tidal tail. The nucleus is the green filled triangle. The dashed line represents the mean trend seen in the colormag diagrams.

• Figure 9; Optical-infrared color-color diagrams. The upper left panel shows the 8 um to 24 um dust continuum ratio versus the 7.7 um PAH line to the 8 um dust continuum. The PAH band strength is estimated by removing the starlight and dust continuum from the 8 um measurements. The upper right panel shows the infrared FPAH to F24um color versus the infrared F3.6um to FPAH color. The lower left panel shows the r'-band to infrared 3.6 um ratio versus the g'-band to r'-band ratio. The lower right panel shows the optical U-band to infrared 24 um color to infrared FPAH to F24um color. The filled triangle denotes the nucleus (lower left of figure); filled circles indicate the disk locations, and filled squares the super star clusters in the tidal tail. The reddening vector is indicated in both panels.