NGC 404 star-forming ring

NGC 404, a rejuvenated lenticular galaxy
on a merger-induced, blueward excursion into the green valley

David A. Thilker11affiliation: Center for Astrophysical Sciences, The Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA , Luciana Bianchi11affiliation: Center for Astrophysical Sciences, The Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA , David Schiminovich22affiliation: Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA , Armando Gil de Paz33affiliation: Departamento de Astrofísica y CC. de la Atmósfera, Universidad Complutense de Madrid, Avda. de la Complutense, s/n, E-28040 Madrid, Spain , Mark Seibert44affiliation: Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA ,
Barry F. Madore44affiliation: Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA , Ted Wyder55affiliation: California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125, USA , R. Michael Rich66affiliation: Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095-1547, USA , Sukyoung Yi77affiliation: Department of Astronomy, Yonsei University, Seoul 120-749, Korea , Tom Barlow55affiliation: California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125, USA , Tim Conrow55affiliation: California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125, USA , Karl Forster55affiliation: California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125, USA , Peter Friedman55affiliation: California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125, USA , Chris Martin55affiliation: California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125, USA , Patrick Morrissey55affiliation: California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125, USA , Susan Neff88affiliation: Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA , and Todd Small55affiliation: California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125, USA

We have discovered recent star formation in the outermost portion (1–4 ) of the nearby lenticular (S0) galaxy NGC 404 using GALEX UV imaging. FUV-bright sources are strongly concentrated within the galaxy’s HI ring (formed by a merger event according to del Rio et al.), even though the average gas density is dynamically subcritical. Archival HST imaging reveals resolved upper main sequence stars and conclusively demonstrates that the UV light originates from recent star formation activity. We present FUV, NUV radial surface brightness profiles and integrated magnitudes for NGC 404. Within the ring, the average star formation rate surface density () is M yr kpc. Of the total FUV flux, 70% comes from the HI ring which is forming stars at a rate of M yr. The gas consumption timescale, assuming a constant SFR and no gas recycling, is several times the age of the Universe. In the context of the UV-optical galaxy CMD, the presence of the SF HI ring places NGC 404 in the green valley separating the red and blue sequences. The rejuvenated lenticular galaxy has experienced a merger-induced, disk-building excursion away from the red sequence toward bluer colors, where it may evolve quiescently or (if appropriately triggered) experience a burst capable of placing it on the blue/star-forming sequence for up to 1 Gyr. The green valley galaxy population is heterogeneous, with most systems transitioning from blue to red but others evolving in the opposite sense due to acquisition of fresh gas through various channels.

Subject headings:
galaxies: evolution — galaxies: structure — galaxies: elliptical and lenticular, cD — galaxies: interactions — galaxies: individual(NGC 404)
slugcomment: To appear in Astrophysical Journal Letters

1. Introduction

Strateva et al. (2001) used an early SDSS galaxy catalog to demonstrate that the distribution of galaxies in color space is bimodal, and correlated with galaxy morphology. Galaxies populate separate red and blue sequences in a ( - ) versus color-magnitude diagram, CMD (Baldry et al. 2004). Evolution of galaxies from the blue sequence locus of actively star-forming systems to the red sequence occurs via transition through an intermediate CMD zone, christened the green valley (Martin et al. 2005). Bell et al. (2004) and Faber et al. (2007) have both shown that the red sequence has grown in mass over the period from to . Given that the color bimodality is driven principally by star formation activity and UV bands are an excellent tracer of recent star formation, it is not surprising that the galaxy color sequences are especially well-separated in the UV-optical CMD (see Wyder et al. 2007, hereafter W07). GALEX proved instrumental in characterising the incidence of green valley transition galaxies (W07; Martin et al. 2007, hereafter M07) and understanding their evolution (M07, Schiminovich et al. 2007) from star-forming systems (Salim et al. 2007) to “red and dead” galaxies.

The effect of gas removal, and the subsequent quenching of SF, has been modeled (M07) in the context of galaxies evolving from the blue sequence to the red sequence across the green valley. However, the influence of late addition of gas to red sequence galaxies has received little attention. Contrary to classical expectations, galaxies of the types predominately populating the red sequence (elliptical and lenticular, S0) sometimes are associated with gaseous reservoirs, especially if they are in a low density environment rather than within a cluster (Morganti et al. 2008). Oosterloo et al. (2007) showed the structure of such gas is varied, with some regularly-rotating disks and a complement of extended, offset, even tail-like morphologies – suggesting a diversity in origin. Both galaxy mergers and IGM accretion are viable mechanisms. The presence of centralized star formation in these early-type galaxies (ETGs) populating the red sequence has been associated with low angular momentum sources (such as retrograde mergers) because gas can be efficiently transported to the remnant center and consumed (Serra et al. 2008), leaving behind minimal HI. On the other hand, prograde mergers of a red sequence galaxy with a gas rich object may be the dominant mechanism of forming massive, extended HI distributions around ETGs.

(catalog NGC 404) is a prime target for studies addressing the structure and evolution of field S0 galaxies. It is particularly interesting because it is the nearest lenticular galaxy, lying just outside the Local Group at an estimated distance of 3.1–3.3 Mpc (Karachentsev et al. 2002, Tonry et al. 2001). (catalog NGC 404) is presently isolated in a zone of radius 1.1 Mpc (Karachentsev & Markarov 1999). Although the galaxy is not affected by a cluster environment (as is true for many S0s), it may still have a complex history. Karachentsev & Markarov (1999) suggested (catalog NGC 404) represents the end product in the coalescence of a small galaxy group, having accreted with all other (less massive) group members. At least one merger may have occurred in the recent past (1 Gyr) and be fundamentally responsible for the current UV morphology. del Rio et al. (2004) argue that a large, disk-like, neutral atomic hydrogen (HI) ring surrounding (catalog NGC 404) is the remnant of a merger with a dwarf irregular galaxy which took place some 900 Myr ago, according to their kinematic estimation. Our GALEX observations revealed that this HI ring is now forming stars. However surprising, this rather late discovery is understandable post facto since (catalog NGC 404) is nearly hidden in the glare of red supergiant Beta Andromedae (Mirach), 406 to the south east of the galaxy. This bright foreground star makes it difficult to image the faint surface brightness portions of (catalog NGC 404) at red wavelengths (including H), and the S0 galaxy became colloquially known as ”Mirach’s Ghost”.

In this letter, we present evidence for star formation in (catalog NGC 404)’s outer disk-like HI ring. We refrain from detailed interpretation of UV properties of the inner disk and bulge. Section 2 describes our GALEX observations. Section 3 contains our data analysis. We conclude with discussion in Section 4.

2. GALEX Observations

We imaged NGC 404 with GALEX for 13463 seconds distributed over 11 visits during Fall 2008 in both the far- and near-ultraviolet (FUV, NUV) bands as part of the Nearby Galaxies Survey (NGS). Our observations were coadded by the GALEX pipeline. The resulting deep FUV[NUV] image has 4.2[5.3]″resolution (Morrissey et al. 2007).

The FUV band of GALEX effectively suppresses glare from Mirach and thus provides an unprecedented look at the star-forming stellar population of (catalog NGC 404). However, UV imaging can be susceptible to extinction, effectively censoring the most embedded star formation events (Calzetti et al. 2005, Thilker et al. 2007b). In the outskirts of (catalog NGC 404) the expected extinction is thought to be low overall, as we describe in Section 3.1.

Figure 1 (top) presents a side-by-side comparison of red POSS-II, GALEX FUV, and HI (WHISP, van der Hulst et al. 2001) imaging for a wide field centered on NGC 404, encompassing the galaxy’s entire low HI column density disk (detected until a radial distance of 800, 12.8 kpc). The red light image gives no indication regarding the presence of the HI disk. However, we find that the main HI ring (between radii of 100–400, 1.6–6.4 kpc) contains many FUV-bright sources, far in excess of the number expected from the background galaxy population. These GALEX sources are frequently unresolved or only marginally resolved, but often delineate larger aggregate structures (sizes of 0.1 kpc to at least 2 kpc). The large scale UV structures are correlated with the most prominent areas of HI, though sometimes with a positional offset between associated features. The UV/HI morphology is suggestive of spiral waves triggering the star formation. We also note that at least in the UV, the most significant HI peaks do not show as prominent SF sites. Some of the high regions may be on the verge of forming the next generation of stellar clusters, but haven’t yet. We have plans to check for molecular gas concentrations matching the peaks.

We display a color-composite GALEX image of NGC 404 in the bottom panel of Fig. 1. The inner disk and bulge of NGC 404 appear prominently in the NUV-band, with average = 1.8 ABmag within (102), as is typical for an S0 galaxy (Donas et al. 2007). The inner disk shows minimal substructure at 5″(80 pc) GALEX resolution, though other studies have described dust clouds (Tikhonov et al. 2003), molecular gas (Sage 1990, Wiklind & Henkel 1990) and an ionized disk (Plana et al. 1998) within 200 pc of the LINER nucleus. The single most luminous FUV source in the galaxy occupies the nuclear area and is known to contain one dominant and several faint clusters of massive stars (Maoz et al. 1995, 1998). The most remarkable aspect of the color image in Fig. 1 is the distribution of blue (FUV-bright) sources occupying the main SF HI ring. Typical FUV luminosity of individual clumps in this ring is erg s ( = 23.0 ABmag, or = -5.6 at 3.3 Mpc). All UV-related measurables in this paper have been corrected only for Milky Way extinction, with = 0.059 mag (Schlegel et al. 1998). Comparing intrinsic UV color to instantaneous burst Starburst99 models (Leitherer et al. 1999) we estimate most sources have age 30 Myr – 1 Gyr and corresponding stellar mass 10–10 M. There is a sharp decline to the surface density of GALEX sources having blue beyond a radius of 400″. The radial profile of del Rio et al. (2004) indicates the average column density in this zone beyond the main ring is cm. Two areas of exceptionally blue, yet diffuse FUV are seen – NE of the SF ring and overlapping with the ring to the ESE. Their position within a larger filamentary network covering the GALEX field of view suggests they are attributable to Galactic cirrus.

3. Analysis and Results

3.1. Global structure

The top panel of Fig. 2 shows background-subtracted, foreground-extinction corrected UV surface brightness profiles and growth curves measured for NGC 404 after masking of foreground stars and distant, unrelated galaxies. The bottom panel of Fig. 2 presents as a function of galactocentric distance. Table 1 lists integrated magnitudes and several quantities derived after folding in corollary data.

We neglect any average internal extinction, supported by inspection of Spitzer 24m imaging of the SF ring obtained as part of the LVL Survey (Lee et al. 2009, Dale et al. 2009). Very few of the FUV-bright sources in NGC 404’s ring have candidate 24m counterparts. Indeed, association in these cases may result from confusion of dusty background galaxies with UV ring clumps. Our extinction assumption is also supported by Prescott et al. (2007) who show that the fraction of highly obscured SF regions in ordinary galaxy disks is very small (). Because we focus on a comparatively low density, outer-disk environment, this is likely even more true in the NGC 404 ring (with at most a few significantly obscured SF complexes).

Fig. 2 shows that: (1) the main HI ring, at galactocentric distance =100-400, has an average ABmag/sq.arcsec; (2) appears to slowly decline with increasing radius in the ring, from about 2 to 0.2, probably reflecting contamination from an underlying exponential disk at least for smaller radii; (3) UV color for the inner disk/bulge is nearly constant at =2.2 except for the nuclear area where FUV surface brightness increases (perhaps due to the LINER, or stronger UV-upturn in central regions of the bulge, e.g. Ohl et al. 1998), bringing down to 1.1. From the curve of growth, we determine that 70% of the total FUV luminosity ( = erg s, corresponding to =14.9) in NGC 404 comes from the SF HI ring defined in (1). The HI ring has a SFR of 0.0025 M yr, adopting the SFR calibration of Salim et al. (2007, their Eq. 8) for a Chabrier IMF over 0.1-100 M.

3.2. HST detection of a resolved young, stellar population

Very deep F606W (39000s) and F814W (75400s) WFPC2 imaging of NGC 404 was obtained as part of ANGST (Dalcanton et al. 2009) and serendipitously samples a subsection of the SF ring ( 160, 2.6 kpc). We obtained the ANGST public-release photometric catalog of resolved stars from the Hubble Legacy Archive (HLA). Coadded images in F606W and F814W bands were retrieved from the ST-ECF HST Archive. At the color of the main sequence, ANGST observations of NGC 404 are 100% complete for sources brighter than F814W = 25.5 mag and 50% complete down to 26.7 mag. This depth is sufficient to recover all massive main sequence stars.

The NGC 404 ANGST dataset will be described in a dedicated paper (Thilker et al. in prep.) but we note the following after initial image inspection: (1) there is minimal surface density enhancement within UV clumps, consistent with a single star or few stars emitting significant UV (cf. Gil de Paz et al. 2007); (2) occasional evidence for diffuse, nebular (H) emission in the F606W band is seen; (3) the overall distribution of resolved stars declines in surface density as a function of galactocentric distance, indicating the continued presence of an older, evolved disk (noted by Tikhonov et al. (2003) for a different WFPC2 field) at large underlying the ring; and (4) a small minority of the UV clumps may be contaminating sources such as background galaxies.

The HST data confirm that the UV light detected by GALEX originates from a young stellar population. CMD analysis of the ANGST catalogs in comparison to theoretical isochrones (Marigo et al. 2008) shows that in the UV clumps we detect main sequence stars ranging in mass from 5–40 M, post turn-off stars (including blue loop), and a background of RGB/AGB stars. Post turn-off stars in the 100-300 Myr age range are also found outside of the UV clumps, suggesting stars from dispersed clusters may be present in the field.

3.3. Star formation law & threshold considerations

del Rio et al. (2004) showed that gas surface density in the NGC 404 ring is subcritical in terms of the azimuthally-averaged parameter. Our data indicate that SF occurs in this environment, having average = 1.2 M pc between =100-400. This is not surprising given other low density SF detected by GALEX (XUV-disks, Thilker et al. 2007; ordinary spirals, Boissier et al. 2007; low-surface-brightness galaxies, Wyder et al. 2009; ETGs, Donovan et al. 2009). Local conditions must still be conducive to massive star formation. Indeed, clumps in the HI ring do reach 4 M pc.

However, the average SFR surface density in NGC 404’s ring ( M yr kpc) is remarkably low and provides further constraint on the SF law at low density. Even assuming negligible molecular content, the NGC 404 ring falls 1 dex below the traditional Kennicutt (1998) (log , log ) correlation. The implied gas consumption timescale is (Hubble time, 1/), without gas recyclying. Equivalently, we infer SF efficiency of yr (0.16% over 100 Myr, or less than typical in galactic disks). The NGC 404 data is roughly consistent with the theoretical SF law of Krumholz et al. (2009), including a downturn in SF efficiency at low density due to a suppressed molecular fraction. The remaining offset (although small) is consistent with not accounting for a small contribution of molecular gas in the cloud cores of the ring – it must be comparatively rare, but still present. This also true for the Wyder et al. (2009) sample of LSB galaxies.

3.4. Backwards evolution into the green valley

In Figure 3 we plot the logarithm of volume density of galaxies in the UV-optical galaxy CMD. W07 fits to the red and blue (M, ) sequences are marked. The green valley is the transitional region between these sequences. Conventionally most green valley objects are thought to be evolving from the blue to the red sequence, after cessation of star formation activity. The GALEX photometry presented above is used to mark the position of NGC 404 in the galaxy CMD, both with (green) and without (red) the contribution of the HI ring. Optical magnitudes in both cases were determined by extrapolating the -band, 84.6 diameter aperture measurement of Sandage & Visvanathan (1978) with the -band surface brightness profiles of Tiknohov et al. (2003).

Assuming NGC 404’s HI ring originates from a recent merger (del Rio et al. 2004), then the galaxy has evolved from a red sequence object and moved backwards into the green valley. We do not yet have a detailed recent SFH to know if is already returning to the red sequence or whether it will continue to evolve bluewards. At the present SFR, it could indefinitely continue quiescently building (SFR/M = -11.4) a low surface brightness outer disk. Alternatively, if an epoch of enhanced SF were triggered perhaps by another encounter, consumption of the gas reservoir could position the galaxy on the blue/S-F sequence (SFR/M=-9.4) for 1 Gyr. If the available HI in the ring were eventually all converted into stars, it could contribute an additional 20% to the stellar mass of NGC404 (currently M derived from SED fitting of UV-NIR integrated photometry), while substantially decreasing the bulge-to-disk mass ratio.

4. Discussion

Star formation and associated gas are no longer viewed as uncommon in lenticular and elliptical galaxies, owing to ever more sensitive UV and HI imaging surveys. Residual star formation is thought to be present in 10–30% of the early-type galaxies examined with GALEX (Yi et al. 2005, Donas et al. 2007, Schawinski et al. 2007, Kaviraj et al. 2007), even after excluding classical UV upturn candidate galaxies from the sample. An external source of gas (accretion or mergers) very likely supplements the SF fuel available via recycling from stellar mass loss. HI imaging for ETG samples supports this conclusion, frequently revealing extended gaseous distributions (Morganti et al. 2008). What remains to be determined is the long term effect of externally-fueled SF on the morphology of red-and-dead galaxies and on the appearance of the UV-optical galaxy CMD. Sometimes the gas is quickly consumed near the galaxy center (Serra et al. 2008), having little net effect on morphology and a very short-lived movement within the galaxy CMD. Activity of this sort is the “frosting” variety described by Trager et al. (2000), though Schawinski et al. (2009) also describe ETGs with rather high centralized SFRs ( M yr). We have shown that rejuvenation of large-scale disk formation is another possible outcome, as discovered in NGC 404 at a very low level. NGC 404 is classified as a Type 1 XUV-disk using the criteria of Thilker et al. (2007). Similar cases have been reported by Cortese & Hughes (2009), Donovan et al. (2009) and Rich & Salim (2009). Rejuvenation events may effectively transplant red sequence galaxies to the green valley and blue sequence. We note that E/S0 galaxies have been detected already on the blue sequence (Kannappan et al. 2009, Schawinski et al. 2009). NGC 404 represents a possible example of this transition underway.

We conclude that the galaxy CMD transition zone known as the green valley represents a heterogeneous population of objects, with many evolving from blue to red but others going in the opposite direction. Stochastic excursions into the green valley from the red-sequence, driven by acquisition of fresh gas for star formation, are observed. Traffic through the green valley is not one-way. NGC 404 confirms that the merger of ETGs and gas-rich dwarfs are one mechanism establishing this diversity. This implies UV imaging is fundamentally required to place individual ETGs into an accurate evolutionary context, assessing whether they are red and dead (at least for the moment), experiencing residual star formation in the galaxy center, or entering a rejuvenated phase of disk building fueled by a long-lasting gas reservior. In fact, UV imaging is an effective means of detecting such potentially transformational reservoirs.

GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in April 2003. We gratefully acknowledge NASA’s support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. This research has made use of the NASA/IPAC Extragalactic Database (NED). We acknowledge the usage of the HyperLeda database ( The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. Some images presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). Facilities: GALEX, HST (WFPC2), NRAO (VLA), WSRT.


  • Baldry et al. (2004) Baldry, I. K., Glazebrook, K., Brinkmann, J., Ivezić, Ž., Lupton, R. H., Nichol, R. C., & Szalay, A. S. 2004, ApJ, 600, 681
  • Bell et al. (2004) Bell, E. F., et al. 2004, ApJ, 608, 752
  • Boissier et al. (2007) Boissier, S., et al. 2007, ApJS, 173, 524
  • Cardelli et al. (1989) Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245
  • Calzetti et al. (2005) Calzetti, D., et al. 2005, ApJ, 633, 871
  • Cortese & Hughes (2009) Cortese, L., & Hughes, T. M. 2009, MNRAS, 1412
  • Dalcanton, J. et al. (2009) Dalcanton, J. et al. 2009, ApJ submitted
  • Dale et al. (2009) Dale, D. A., et al. 2009, ApJ, 703, 517
  • del Río et al. (2004) del Río, M. S., Brinks, E., & Cepa, J. 2004, AJ, 128, 89
  • Donas et al. (2007) Donas, J., et al. 2007, ApJS, 173, 597
  • Donovan et al. (2009) Donovan, J. L., et al. 2009, AJ, 137, 5037
  • Faber et al. (2007) Faber, S. M., et al. 2007, ApJ, 665, 265
  • Gil de Paz et al. (2007) Gil de Paz, A., et al. 2007, ApJ, 661, 115
  • Jarrett et al. (2003) Jarrett, T. H., Chester, T., Cutri, R., Schneider, S. E., & Huchra, J. P. 2003, AJ, 125, 525
  • Kannappan et al. (2009) Kannappan, S. J., Guie, J. M., & Baker, A. J. 2009, arXiv:0903.3695
  • Karachentsev & Makarov (1999) Karachentsev, I. D., & Makarov, D. I. 1999, Galaxy Interactions at Low and High Redshift, 186, 109
  • Karachentsev et al. (2002) Karachentsev, I. D., et al. 2002, A&A, 389, 812
  • Kaviraj et al. (2007) Kaviraj, S., et al. 2007, ApJS, 173, 619
  • Kennicutt (1998) Kennicutt, R. C., Jr. 1998, ApJ, 498, 541
  • Lee et al. (2009) Lee, J. C., et al. 2009, ApJ, 706, 599
  • Leitherer et al. (1999) Leitherer, C., et al. 1999, ApJS, 123, 3
  • Maoz et al. (1995) Maoz, D., Filippenko, A. V., Ho, L. C., Rix, H.-W., Bahcall, J. N., Schneider, D. P., & Macchetto, F. D. 1995, ApJ, 440, 91
  • Maoz et al. (1998) Maoz, D., Koratkar, A., Shields, J. C., Ho, L. C., Filippenko, A. V., & Sternberg, A. 1998, AJ, 116, 55
  • Marigo et al. (2008) Marigo, P., Girardi, L., Bressan, A., Groenewegen, M. A. T., Silva, L., & Granato, G. L. 2008, A&A, 482, 883
  • Martin et al. (2007) Martin, D. C., et al. 2007, ApJS, 173, 342
  • Morganti et al. (2008) Morganti, R., et al. 2008, The Evolution of Galaxies Through the Neutral Hydrogen Window, 1035, 129
  • Morrissey et al. (2007) Morrissey, P., et al. 2007, ApJS, 173, 682
  • Oosterloo et al. (2007) Oosterloo, T. A., Morganti, R., Sadler, E. M., van der Hulst, T., & Serra, P. 2007, A&A, 465, 787
  • Plana et al. (1998) Plana, H., Boulesteix, J., Amram, P., Carignan, C., & Mendes de Oliveira, C. 1998, A&AS, 128, 75
  • Prescott et al. (2007) Prescott, M. K. M., et al. 2007, ApJ, 668, 182
  • Rich & Salim (2009) Rich, R. M., & Salim, S. 2009, Bulletin of the American Astronomical Society, 41, 252
  • Sage (1990) Sage, L. J. 1990, A&A, 239, 125
  • Salim et al. (2007) Salim, S., et al. 2007, ApJS, 173, 267
  • Sandage & Visvanathan (1978) Sandage, A., & Visvanathan, N. 1978, ApJ, 225, 742
  • Schawinski et al. (2007) Schawinski, K., et al. 2007, ApJS, 173, 512
  • Schawinski et al. (2009) Schawinski, K., et al. 2009, arXiv:0903.3415
  • Schiminovich et al. (2007) Schiminovich, D., et al. 2007, ApJS, 173, 315
  • Schlegel et al. (1998) Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525
  • Serra et al. (2008) Serra, P., Trager, S. C., Oosterloo, T. A., & Morganti, R. 2008, A&A, 483, 57
  • Strateva et al. (2001) Strateva, I., et al. 2001, AJ, 122, 1861
  • Thilker et al. (2007) Thilker, D. A., et al. 2007, ApJS, 173, 538
  • Thilker et al. (2007) Thilker, D. A., et al. 2007b, ApJS, 173, 572
  • Tikhonov et al. (2003) Tikhonov, N. A., Galazutdinova, O. A., & Aparicio, A. 2003, A&A, 401, 863
  • Tonry et al. (2001) Tonry, J. L., Dressler, A., Blakeslee, J. P., Ajhar, E. A., Fletcher, A. B., Luppino, G. A., Metzger, M. R., & Moore, C. B. 2001, ApJ, 546, 681
  • Trager et al. (2000) Trager, S. C., Faber, S. M., Worthey, G., & González, J. J. 2000, AJ, 120, 165
  • van der Hulst et al. (2001) van der Hulst, J. M., van Albada, T. S., & Sancisi, R. 2001, Gas and Galaxy Evolution, 240, 451
  • Wiklind & Henkel (1990) Wiklind, T., & Henkel, C. 1990, A&A, 227, 394
  • Wyder et al. (2007) Wyder, T. K., et al. 2007, ApJS, 173, 293
  • Wyder et al. (2009) Wyder, T. K., et al. 2009, arXiv:0903.3015
  • Yi et al. (2005) Yi, S. K., et al. 2005, ApJ, 619, L111
Figure 1.— DSS2-red (top-left), GALEX FUV (top-center), HI (top-right) imaging of a wide-field centered on NGC 404, plus a detailed FUV, NUV color-composite image of NGC 404 (bottom). The FUV ( = 1538.6 Å) imaging reveals star formation in the ring. The wide-field panels (at top) span 0.5°0.5°(27.3 kpc) with N up and E left. The GALEX color-composite was created by assigning FUV to the blue channel, NUV ( = 2315.7 Å) to the red channel, and an energy-weighted average of FUV and NUV to green channel. FUV-bright sources appear blue/white, including the majority of the detections in the SF ring. The inner disk and bulge appears yellow because it is NUV-bright, dominated by older stars than the SF ring. Dichroic reflections appear as yellow doughnuts of varied size near bright foreground stars (including Mirach, SE of the galaxy). The color-composite field is 22.85′21.80′(20.819.8 kpc).
Figure 2.— GALEX radial profile analysis for NGC 404. (top) Average surface brightness and corresponding curve of growth as a function of galactocentric distance for the FUV (blue solid) and NUV (red dashed) GALEX bands. The 1 confidence intervals for the surface brightness profiles, including the uncertainty from sky subtraction, are plotted with thin color-coded lines. (bottom) Azimuthally-averaged FUV-NUV color with error limits (dotted lines), which are dominated by sky level uncertainty.
Figure 3.— UV-optical galaxy CMDs [left, (M,); right, (M,)] adapted from W07, upon which we have marked the position of NGC 404 both with and without the contribution of flux from SF HI ring, using green and red dots respectively. In the (M,) CMD we overplot the W07 fits to the red and blue galaxy sequences. NGC 404 falls into the green valley when the ring is included. Galaxy volume density is greyscaled over a range of 6 dex, with contours drawn every 0.5 dex.
Quantity Value Unit Ref
Hubble Type SA(s)0- (1)
Morph. Code, -2.80.6 (2)
Spectral (AGN) Type LINER (1)
RA (J2000) 01h 09m 27.010s (1)
DEC (J2000) +35d 43m 04.20s (1)
Heliocentric Velocity -489 km s (1)
DistanceaaWe adopted 3.3 Mpc for consistency with del Rio et al. (2004). 3.3 Mpc (3)
20314 arcsec (2)
arcsec (3)
Inclination, 0–11 deg (2,3)
M (3)
M (4)
M (3)
85 M/L (3)
0.42 M/L (3)
DEF(HI), HI deficiencybbBased on the Haynes & Giovanelli (1984) definition. -0.54 (3)
0.22 (3,4)
Galactic 0.059 mag (1)
14.89 ABmag (4)
13.68 ABmag (4)
9.51 ABmag (5,6)
16.20 ABmag (4)
14.39 ABmag (4)
9.74 ABmag (5,6)
erg s (4)
M yr (4)
M yr (4)
M yr (4)
Gas consumption time, 59 Gyr (4)
yr (4)

Note. – (1) NED, (2) HyperLEDA, (3) del Rio et al. (2004), (4) this paper, (5) Sandage & Visvanathan (1978), (6) Tikhonov et al. (2003)

Table 1Properties of NGC 404
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description