NGP01 The bright (R=16.59, K=13.77) counterpart is identified as 
NGP01  2MASSX J13412738+4042166 with a redshift of z=0.088. The optical data 
NGP01  show a disc-dominated galaxy with wide arms, typical to late spirals, bar
NGP01  structure identified with galfit and a somewhat disturbed morphology at 
NGP01  the southern edge, typical to e.g. merger remnants. HYPERZ fits perfectly
NGP01  a fully evolved (nominally 15-Gyr old) grasil Sc template, the ERR03 
NGP01  models fit a cirrus-dominated SED, while the SDSS spectrum shows strong 
NGP01  H{alpha} emission. The FIR points alone - detections at 150 and 170um, 
NGP01  but only an upper limit at 90um - suggest a strong cool cirrus component.
NGP01  We also note that there is another bright star-forming galaxy at exactly 
NGP01  the same redshift just outside the FIR detection circle, 2.5arcmin 
NGP01  (or 250kpc projected distance) away from the adopted counterpart.
NGP02 There is a significant concentration of K~15-17mag galaxies within and 
NGP02  just outside the ISOPHOT area - there are four galaxies with K<16mag and 
NGP02  a further four with K<17mag. None has spectroscopy available and none of 
NGP02  the galaxies within the detection circle produces satisfactory SED fits 
NGP02  when ISOPHOT data are included. However, the four brightest galaxies all 
NGP02  have optical/NIR photometric redshifts of z~0.28 , along with further 
NGP02  three fainter ones. They include a tidally disrupted interacting pair, 
NGP02  two Sb-type SEDs, as well as two bright early-type galaxies. A 
NGP02  combination of two or three of the disc galaxies at this redshift is well
NGP02  able to produce the required FIR flux. An exact identification of 
NGP02  NGP02 is thus ambiguous, though a mixed origin is very likely.
NGP03 The bright (R=17.12, K=14.20) counterpart is identified as 
NGP03  2MASSX J13422216+4022017 at z=0.131. It has two or three fainter galaxies
NGP03  clearly in close interaction. galfit modelling shows a large 
NGP03  bulge-dominated disc of 6.9kpc scalelength with wide spiral arms and the
NGP03  subtraction of bulge and disc components reveals a ring-like structure 
NGP03  extending towards two of the companions, and possibly bar-like structure 
NGP03  at the nucleus. Again, the SDSS spectrum shows strong star formation. The
NGP03  FIR SED is now warmer (detected at 90um but not at 180um) and our 
NGP03  best-fitting SED template is, indeed, that of a prototype interacting 
NGP03  starburst galaxy NGC 6090, further corroborating its starburst nature. 
NGP03  Note that this template has more power in the cooler FIR range than an 
NGP03  M82 SED would have. The ERR03 model is similar to NGP01.
NGP04 There are no bright (K<16, R<20) galaxies in this field. The FIR detection
NGP04  is 130arcsec away from an X-ray detected galaxy cluster RX J1342.8+4028 
NGP04  at z=0.699. The HYPERZ fits to SDSS and RIK data find a large 
NGP04  concentration of z~0.6 galaxies in the ISOPHOT area, which most likely 
NGP04  belong to the cluster. Specifically, there are three red galaxies within 
NGP04  the detection circle which fit quite well an Arp 220 SED at those 
NGP04  redshifts - and the fits are even better if the FIR is a sum of two of 
NGP04  them. Two of these sources, including the brightest object in the field, 
NGP04  are clearly disturbed objects. A sum of faint galaxies is thus the 
NGP04  likeliest counterpart for the ISOPHOT detection.
NGP05 The brightest galaxy is a morphologically disturbed barred late-type 
NGP05  spiral; there are no spectra available. The galaxy fits reasonably an 
NGP05  evolved Sc template at z~0.25 , though it would need ~two times more FIR 
NGP05  flux to fit well the FIR points. Other galaxies may thus contribute to 
NGP05  the FIR flux; and indeed there are two other galaxies (K<16.6mag) with 
NGP05  photometric redshifts at z~0.2 , best-fitting SEDs (when fit is done 
NGP05  excluding the ISOPHOT points) of early- and late-type spirals and disc 
NGP05  morphologies. A confused counterpart is thus likely.
NGP06 The brightest galaxy is 2MASSX J13430669+4014314 with an SDSS redshift of 
NGP06  z=0.163. Both the optical spectrum and optical/NIR SED indicate an 
NGP06  Sb-type, but the SED including all three FIR points does not fit well any
NGP06  of our templates at that redshift - the NGP 6090 template gives a 
NGP06  reasonable fit at the 2{sigma} error levels of the FIR fluxes, but the 
NGP06  optical spectrum is not that of a starburst. It is possible that the FIR 
NGP06  detection come from some combination of a warm (contributing to the 
NGP06  90um band) and a cold object (the 180um flux). There are also two 
NGP06  fainter interacting pairs in the detection circle which both would 
NGP06  reasonably fit an Arp 220 template at z~0.5-0.6 , contributing to the 90
NGP06  and 150um fluxes in that case. The identification thus remains ambiguous.
NGP07 Juvela et al. (2000A&A...360..813J) list this object with two positions 
NGP07  in the 90um catalogue (NGP07 and NGP08, separated by 20arcsec) and a 
NGP07  single detection in 150 and 180um, suggesting a complex origin for the 
NGP07  FIR flux. There are four fairly bright galaxies in the area, though only 
NGP07  one K<16mag. By far the brightest appears to be an early-type spiral or 
NGP07  lenticular while the three others are also all early-type discs. None of 
NGP07  these alone fit the SED templates over all the wavelength range. A 
NGP07  confused FIR source, in between z~0.25-0.40 based on photometric 
NGP07  redshifts, is highly probable.
NGP09 The two brightest galaxies in the region, only one is K<16mag, are disc 
NGP09  galaxies, but we cannot fit well either of them and the FIR flux is too 
NGP09  strong to be associated even with their sum. There are, however, several 
NGP09  very red galaxies giving acceptable fits to ULIRG templates in a wide 
NGP09  redshift range of z~0.2-0.8. We also note that this is one of three 
NGP09  sources in the sample of 22 NGP FIR targets which do not have quality 
NGP09  flag values of q>=3 in any FIR band.
NGP10 There are no galaxies brighter than K=16mag in the field and no object 
NGP10  provides an acceptable HYPERZ fit. There are, however, half a dozen 
NGP10  galaxies redder than R-K>4 in the area including two EROs, which could 
NGP10  contribute in combinations at z~0.5-1.0 where their optical/NIR 
NGP10  photometric redshifts place them.
NGP11 No single galaxy fits well the template SEDs, though there are two K~15.5 
NGP11  disc galaxies in the field, the sum of which can explain the FIR points 
NGP11  if both are Sc types at their photometric redshift of z~0.3. They belong
NGP11  to an apparent concentration of galaxies partially inside the ISOPHOT 
NGP11  area. We find, however, another fainter red disturbed galaxy which could 
NGP11  contribute as a higher redshift ULIRG.
NGP12 Four galaxies, all K~16mag or brighter, produce excellent exponential 
NGP12  profiles with galfit and good optical/NIR SED fits to spiral or starburst
NGP12  templates in the range z=0.10-0.19. One, or even two, of them appear to 
NGP12  be interacting with another galaxy. However, none of them fit our full 
NGP12  SED templates alone, though a sum of them could explain the required FIR 
NGP12  flux. To complicate matters, there are four fainter red R-K~4 galaxies in
NGP12  the field, any of which fit reasonably well a full ULIRG template in the 
NGP12  range z=0.4-0.55. The very ambiguous aspect of this source is highlighted
NGP12  by the fact that Juvela et al. (2000A&A...360..813J) list this target as 
NGP12  two objects (NGP12 and NGP13) separated by 23arcsec in the 90um 
NGP12  catalogue, while there is only one detection in the 150um list.
NGP14 There are two bright nearby spirals in the area. The brighter one 
NGP14  (R=17.32, K=14.19) is 2MASSX J13473443+3931515, with an SDSS redshift of 
NGP14  z=0.16. The optical spectrum looks to be of a typical star-forming 
NGP14  galaxy, and the grasil interacting starburst NGC 6090 template gives a 
NGP14  perfect match to the overall SED. The optical image reveals a disc galaxy
NGP14  with a large asymmetric arm. This case would fall into the bright 
NGP14  unambiguous class were it not for the second spiral (K=15.22) which also 
NGP14  fits very well our templates, an evolved Sc galaxy at a photometric 
NGP14  z=0.08. Both galaxies must contribute to the FIR flux.
NGP15 This is one of the most ambiguous cases. There is a tight group of 
NGP15  five-seven galaxies (all fainter than K~15.5mag), including two 
NGP15  interacting pairs, 25arcsec from the FIR location. Two or three of these
NGP15  galaxies together would fit reasonably the FIR points with starburst 
NGP15  templates at z~0.3. Additionally, however, there are three very red 
NGP15  sources elsewhere inside the FIR area. If their elliptical-like 
NGP15  optical/NIR colours are combined with the FIR flux, they fit well ULIRG 
NGP15  templates at z~0.6-0.9. Furthermore, in fact, these sources belong to a 
NGP15  distribution of the largest concentration of EROs found in this follow-up
NGP15  survey, mostly lying just outside the ISO detection circle. NGP15 is one 
NGP15  of the three sources with lower quality flag values of q<3.
NGP16 There are two separate 90um detections just 22arcsec from each other 
NGP16  (NGP16 and NGP17), that are connected with a single detection at longer 
NGP16  wavelengths. A significant concentration of galaxies is seen in the area.
NGP16  There are two disc galaxies in the centre of the area, with early-type 
NGP16  spirals as best-fitting SEDs at photometric redshifts of z~0.2 , but 
NGP16  even a sum of these would not yet explain the FIR fluxes. Intriguingly, 
NGP16  there are also three individual fainter and red (R-K~4) galaxies in the 
NGP16  detection area which each give a good fit to starburst or Arp 220 SEDs at
NGP16  redshifts ranging z=0.1-0.5. One of these is a clear interacting galaxy, 
NGP16  and another a FIRST radio source whose radio flux is consistent with the 
NGP16  fitted Arp 220 SED. Any one of these could be the true counterpart, 
NGP16  unless it is not the confused sum of the brighter galaxies, or a 
NGP16  combination of all. This is a highly ambiguous case.
NGP18 This field is within a galaxy cluster ZwCl 1346.9+3931. Three bright 
NGP18  disturbed spirals are found in the ISOPHOT area, and several more just 
NGP18  outside, all with spectroscopic SDSS redshifts of z=0.13-0.14. The 
NGP18  brightest (R=17.02, K=14.19) of the spirals, 2MASX J13490845+3917219, is 
NGP18  a star-forming galaxy with Seyfert-like emission lines, and the overall 
NGP18  SED actually fits well an evolved Sc template. On the other hand, since 
NGP18  the other spirals in the area must also contribute to the FIR flux 
NGP18  (optical/NIR SEDs are fit with normal spiral and even starburst SEDs), we
NGP18  chose to include NGP18 in the confused sample, rather than the bright 
NGP18  unambiguous sample. It is clear though that the FIR counterpart(s) lies 
NGP18  at the redshift of z~0.13.
NGP19 The ISOPHOT circle does not have very bright galaxies, though there are 
NGP19  many at both sides of K~16mag. The 90um flux is the strongest of the 
NGP19  whole sample, making this our only source with a clearly declining SED 
NGP19  longwards of 100um. Morphologically, according to galfit, two of the 
NGP19  brighter ones are face-on discs with stellar point spread function (PSF) 
NGP19  and/or strong bulge components. Both fit well an Arp 220 template at 
NGP19  z~0.35, though without spectra it is impossible to speculate more about 
NGP19  starbursts or obscured AGN, or to decide between them. Contributions from
NGP19  other galaxies cannot be ruled out either: the second brightest galaxy in
NGP19  the field is a warped interacting disc galaxy, it does not fit any 
NGP19  template by itself, and there are three fainter very red galaxies in the 
NGP19  area giving reasonable fits to ULIRG or ERO templates in redshift ranges 
NGP19  of z~0.3-0.6 .
NGP20 The bright (R=17.75, K=14.80) galaxy in the detection circle has no SDSS 
NGP20  spectra, but it does have a strong HYPERZ fit (chi^2^=0.2 at z=0.137) 
NGP20  with a fully evolved Sc template, consistent with the ERR03 fit as well. 
NGP20  It has an undisturbed disc and a small but bright bulge in the optical. 
NGP20  There is another bright galaxy of early type just outside the field 
NGP20  1.1arcmin away (2MASX J13494050+3907555) which has a known redshift of 
NGP20  z=0.143 making the photometric redshift of the first galaxy, the adopted 
NGP20  counterpart, very plausible.
NGP21 There are no galaxies brighter than K=16 (the bright object seen in Fig. 3
NGP21  is a star), and none of the sources give good SED fits. The brightest 
NGP21  source is a disc galaxy, but no template fits the FIR points. There are 
NGP21  also three very faint EROs in the field which could conceivably 
NGP21  contribute if they have ULIRG type SEDs, though none of them alone. This 
NGP21  FIR source is the third ISO target with a lower quality flag value of 
NGP21  q<3.
NGP22 The only bright galaxy (R=17.70, K=14.52) in the vicinity is the edge-on 
NGP22  disc galaxy SDSS J135054.71+385847.2 at a redshift of z=0.086. The disc 
NGP22  is somewhat warped, though there are no obvious major partners nearby. 
NGP22  The SDSS spectrum shows H{alpha}, though not much else, and the overall 
NGP22  SED fits reasonably the evolved Sc template at that redshift, though the 
NGP22  optical/NIR SED would be better fit with an M82 template. This galaxy is 
NGP22  two-three times less massive than the previous four objects, and the SFR 
NGP22  predicted by both grasil and ERR03 is also smaller, but still a little 
NGP22  higher than ordinary quiescent galaxies. ERR03 again fits a 
NGP22  cirrus-dominated galaxy.
NGP23 This field again holds a significant concentration of bright galaxies. The
NGP23  brightest (R=16.73, K=13.60) galaxy has the galfit profile of an 
NGP23  elliptical or strongly bulge-dominated disc galaxy and it fits reasonably
NGP23  an overall Sb-type SED. The two next brightest galaxies have SDSS spectra
NGP23  (z~0.20) showing star formation, and they are discs, as are two other 
NGP23  bright galaxies, all with optical/NIR spectral shapes consistent with 
NGP23  spirals. Most of these galaxies must contribute toward the total FIR 
NGP23  flux, and the identification thus remains ambiguous.
NGP24 The counterpart galaxy of this FIR source is the most nearby galaxy in our
NGP24  sample, UGC 08793 at a redshift of z=0.0081 and it extends over 1.5arcmin
NGP24  on the sky. Its IR luminosity is more than two orders of magnitude less 
NGP24  than the other bright sample galaxies above. The SDSS spectrum of the 
NGP24  centre shows a typical late-type spiral spectrum, NED classifies it as 
NGP24  Sd, and our overall SED shape is well fit with a template of local Scd 
NGP24  dwarf galaxy NGC 6946. This is the only case where ERR03 suggest a pure 
NGP24  cirrus spectrum. It has numerous bright HII regions, several small 
NGP24  satellite galaxies or giant HII regions and the disc appears slightly 
NGP24  warped.
NGP25 This case is somewhat ambiguous though there is a single bright galaxy 
NGP25  (R=16.65, K=13.61) in the ISOPHOT area: it appears to be an early-type 
NGP25  galaxy (Sa template fits the optical/NIR SED), with some evidence of 
NGP25  structure beneath a galfit de Vaucoulers profile. It does not have a 
NGP25  spectrum, but there is a galaxy of the same size and brightness 47arcsec
NGP25  away to the NE just outside the detection circle. Its SDSS redshift is 
NGP25  z=0.118 and it has a clear disc-like galfit profile, and the best-fitting
NGP25  SED is an Sb type. Contributions from (at least) both of these galaxies 
NGP25  would be needed, however, to explain the FIR flux. An Sc-type SED could 
NGP25  fit the overall SED alone but the morphology of neither galaxy favours 
NGP25  this option.