NGC 404, Mirach's Ghost, Galaxy in Andromeda

Total Page:16

File Type:pdf, Size:1020Kb

Load more

NGC 404, Mirach's Ghost, Galaxy in Andromeda NGC 404 is classified as a lenticular galaxy, one that somewhere between a spiral galaxy and an elliptical galaxy. It appears as a round glow with a much brighter center when viewed through a telescope at medium to high power. It is very easy to find because it is so close to the bright star Mirach (both seen in the picture here). Despite the presence of the bright star, the 10th magnitude galaxy is surprisingly easy to see through a telescope of medium or large aperture. The galaxy is about 10 million light years away. Start by finding the Great Square of Pegasus, which rises in the eastern sky during the early fall evenings, is high overhead later in the fall, and sinks in the western sky during early winter. To be sure you know how the square is oriented in the sky, look for the two stars outside the northwest corner of the square (circled in the chart here) that form a small triangle with Scheat. The constellation Andromeda stretches to the northeast from the Great Square, starting at the second-magnitude star Alpheratz. Using the naked eye, look to the east of Alpheratz for the star delta (δ) Andromedae, then move on to the brighter star Mirach. NGC 404 is just 7 arcminutes (about 1/10 of a degree) northeast of Mirach, so the bright star and dim galaxy should be visible together through a telescope, even at high magnification. To avoid the glare of Mirach, you can put it just outside the field of view. From www.skyledge.net by Jim Mazur. Star charts created with Cartes du Ciel. .
Recommended publications
  • And Ecclesiastical Cosmology

    And Ecclesiastical Cosmology

    GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc.
  • Astronomy 2009 Index

    Astronomy 2009 Index

    Astronomy Magazine 2009 Index Subject Index 1RXS J160929.1-210524 (star), 1:24 4C 60.07 (galaxy pair), 2:24 6dFGS (Six Degree Field Galaxy Survey), 8:18 21-centimeter (neutral hydrogen) tomography, 12:10 93 Minerva (asteroid), 12:18 2008 TC3 (asteroid), 1:24 2009 FH (asteroid), 7:19 A Abell 21 (Medusa Nebula), 3:70 Abell 1656 (Coma galaxy cluster), 3:8–9, 6:16 Allen Telescope Array (ATA) radio telescope, 12:10 ALMA (Atacama Large Millimeter/sub-millimeter Array), 4:21, 9:19 Alpha (α) Canis Majoris (Sirius) (star), 2:68, 10:77 Alpha (α) Orionis (star). See Betelgeuse (Alpha [α] Orionis) (star) Alpha Centauri (star), 2:78 amateur astronomy, 10:18, 11:48–53, 12:19, 56 Andromeda Galaxy (M31) merging with Milky Way, 3:51 midpoint between Milky Way Galaxy and, 1:62–63 ultraviolet images of, 12:22 Antarctic Neumayer Station III, 6:19 Anthe (moon of Saturn), 1:21 Aperture Spherical Telescope (FAST), 4:24 APEX (Atacama Pathfinder Experiment) radio telescope, 3:19 Apollo missions, 8:19 AR11005 (sunspot group), 11:79 Arches Cluster, 10:22 Ares launch system, 1:37, 3:19, 9:19 Ariane 5 rocket, 4:21 Arianespace SA, 4:21 Armstrong, Neil A., 2:20 Arp 147 (galaxy pair), 2:20 Arp 194 (galaxy group), 8:21 art, cosmology-inspired, 5:10 ASPERA (Astroparticle European Research Area), 1:26 asteroids. See also names of specific asteroids binary, 1:32–33 close approach to Earth, 6:22, 7:19 collision with Jupiter, 11:20 collisions with Earth, 1:24 composition of, 10:55 discovery of, 5:21 effect of environment on surface of, 8:22 measuring distant, 6:23 moons orbiting,
  • Arxiv:2001.03626V1 [Astro-Ph.GA] 10 Jan 2020 Max Planck Institute for Astronomy K¨Onigstuhl17, 69121 Heidelberg, Germany E-Mail: Neumayer@Mpia.De A

    Arxiv:2001.03626V1 [Astro-Ph.GA] 10 Jan 2020 Max Planck Institute for Astronomy K¨Onigstuhl17, 69121 Heidelberg, Germany E-Mail: [email protected] A

    The Astronomy and Astrophysics Review (2020) Nuclear star clusters Nadine Neumayer · Anil Seth · Torsten B¨oker Received: date / Accepted: date Abstract We review the current knowledge about nuclear star clusters (NSCs), the spectacularly dense and massive assemblies of stars found at the centers of most galaxies. Recent observational and theoretical work suggest that many NSC properties, including their masses, densities, and stellar populations vary with the properties of their host galaxies. Understanding the formation, growth, and ultimate fate of NSCs therefore is crucial for a complete picture of galaxy evolution. Throughout the review, we attempt to combine and distill the available evidence into a coherent picture of NSC 9 evolution. Combined, this evidence points to a clear transition mass in galaxies of 10 M where the characteristics of nuclear star clusters change. We argue that at lower masses, NSCs∼ are formed primarily from globular clusters that inspiral into the center of the galaxy, while at higher masses, star formation within the nucleus forms the bulk of the NSC. We also discuss the coexistence of NSCs and central black holes, and how their growth may be linked. The extreme densities of NSCs and their interaction with massive black holes lead to a wide range of unique phenomena including tidal disruption and gravitational wave events. Lastly, we review the evidence that many NSCs end up in the halos of massive galaxies stripped of the stars that surrounded them, thus providing valuable tracers of the galaxies' accretion histories. Contents 1 Introduction . .2 2 Early studies . .4 2.1 Imaging nuclear star clusters: the Hubble Space Telescope .
  • Mirach's Goblin: Discovery of a Dwarf Spheroidal Galaxy Behind

    Mirach's Goblin: Discovery of a Dwarf Spheroidal Galaxy Behind

    Astronomy & Astrophysics manuscript no. aa c ESO 2018 October 12, 2018 Mirach’s Goblin: Discovery of a dwarf spheroidal galaxy behind the Andromeda galaxy David Martínez-Delgado1, Eva K. Grebel1, Behnam Javanmardi2, Walter Boschin3; 4:5, Nicolas Longeard6, Julio A. Carballo-Bello7, Dmitry Makarov8, Michael A. Beasley4; 5, Giuseppe Donatiello9, Martha P. Haynes10, Duncan A. Forbes11, Aaron J. Romanowsky12; 13 1Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany 2 School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, 19395-5531, Iran 3 Fundación G. Galilei - INAF (Telescopio Nazionale Galileo), Rambla J. A. Fernández Pérez 7, E-38712 Breña Baja (La Palma), Spain 4Instituto de Astrofísica de Canarias (IAC), Calle Vía Láctea s/n, E-38205 La Laguna, Tenerife; Spain 5Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife; Spain 6 Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, F-67000 Strasbourg, France 7Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, 782-0436 Macul, Santiago, Chile 8 Special Astrophysical Observatory, Nizhniy Arkhyz, Karachai-Cherkessia 369167, Russia 9 Nuovo Orione, 72024 Oria, Italy 10Cornell Center for Astrophysics and Planetary Science, Space Sciences Building, Cornell University, Ithaca, NY 14853 , USA 11 Centre for Astrophysics & Supercomputing, Swinburne University of Technology, Hawthorn VIC 3122, Australia 12 Department of Physics & Astronomy, San José State University, One Washington Square, San Jose, CA 95192, USA 13 University of California Observatories, 1156 High Street, Santa Cruz, CA 95064, USA ABSTRACT Context. It is of broad interest for galaxy formation theory to carry out a full inventory of the numbers and properties of dwarf galaxies in the Local Volume, both satellites and isolated ones.
  • Oregon Star Party Level 3 / Advanced Observing List

    Oregon Star Party Level 3 / Advanced Observing List

    Oregon Star Party 2019 Level 3 / Advanced Observing List Howard Banich Welcome to the 2019 OSP Level 3 / Advanced Observing List Each of the fourteen objects on this list has its own page itemizing what it is, why it’s interesting to observe, the minimum size telescope that might needed to see it, and the criteria for a successful observation. Also included are the constellation of each object, coordinates, and a photo showing what the object looks like - all you have to do is find, observe, and record your observations. I hope you enjoy the challenge! Note – you will need your own detailed finder charts for these objects. Paper or computer charts are equally acceptable. Also - star hopping, push-to and goto are all appropriate ways to find these objects. Stretch your skill and imagination - see something new, something unimaginably old, something unexpected • Even though this is a challenging list, you don’t need twenty years of observing experience or a 20-inch telescope to successfully observe ten of these objects. The only way to know if you can see them is to have a look for yourself. • The minimum aperture listed for each object is a rough estimate. The idea is to show approximately the smallest size telescope that might be needed to successfully observe each object. The range is 4-inches to “no idea” this year. • The visibility of each object assumes dark, transparent, steady and non-smoky OSP observing conditions. Requirements to receive a certificate 1. To receive the observing certificate, you need to have descriptive notes and/or sketches that clearly show you observed ten (10) objects on this year’s list.
  • Nearby Early-Type Galactic Nuclei at High Resolution: Dynamical Black

    Nearby Early-Type Galactic Nuclei at High Resolution: Dynamical Black

    Draft version April 13, 2018 Preprint typeset using LATEX style emulateapj v. 04/17/13 NEARBY EARLY-TYPE GALACTIC NUCLEI AT HIGH RESOLUTION { DYNAMICAL BLACK HOLE AND NUCLEAR STAR CLUSTER MASS MEASUREMENTS Dieu D. Nguyen1, Anil C. Seth1, Nadine Neumayer2, Sebastian Kamann3, Karina T. Voggel1, Michele Cappellari4, Arianna Picotti2, Phuong M. Nguyen5, Torsten Boker¨ 6, Victor Debattista7, Nelson Caldwell8, Richard McDermid9, Nathan Bastian3, Christopher C. Ahn1, and Renuka Pechetti1 Draft version April 13, 2018 ABSTRACT We present a detailed study of the nuclear star clusters (NSCs) and massive black holes (BHs) of four of the nearest low-mass early-type galaxies: M32, NGC 205, NGC 5102, and NGC 5206. We measure dynamical masses of both the BHs and NSCs in these galaxies using Gemini/NIFS or VLT/SINFONI stellar kinematics, Hubble Space Telescope (HST ) imaging, and Jeans Anisotropic Models. We detect massive BHs in M32, NGC 5102, and NGC 5206, while in NGC 205, we find only an upper limit. These BH mass estimates are consistent with previous measurements in M32 and NGC 205, while those in 6 NGC 5102 & NGC 5206 are estimated for the first time, and both found to be <10 M . This adds to just a handful of galaxies with dynamically measured sub-million M central BHs. Combining these BH detections with our recent work on NGC 404's BH, we find that 80% (4/5) of nearby, low-mass 9 10 −1 (10 − 10 M ; σ? ∼ 20 − 70 km s ) early-type galaxies host BHs. Such a high occupation fraction suggests the BH seeds formed in the early epoch of cosmic assembly likely resulted in abundant seeds, favoring a low-mass seed mechanism of the remnants, most likely from the first generation of massive 6 stars.
  • Stellar Content of NGC 404 – the Nearest S0 Galaxy

    Stellar Content of NGC 404 – the Nearest S0 Galaxy

    A&A 401, 863–872 (2003) Astronomy DOI: 10.1051/0004-6361:20021819 & c ESO 2003 Astrophysics Stellar content of NGC 404 – The nearest S0 Galaxy N. A. Tikhonov1,2, O. A. Galazutdinova1,2, and A. Aparicio3 1 Special Astrophysical Observatory, Russian Academy of Sciences, N. Arkhyz, KChR 369167, Russia 2 Isaac Newton Institute of Chile, SAO Branch, Russia 3 Instituto de Astrofisica de Canarias, 38200 La Laguna, Tenerife, Spain Recieved 11 December 2000 / Accepted 6 December 2002 Abstract. We report V−band and I−band CCD stellar and surface photometry of the galaxy NGC 404 , taken with HST WFPC2 and the 2.5 m Nordic telescope. The colour-magnitude diagram for the stars in this galaxy is typical of that of spheroidal systems (i.e. it lacks luminous, young stars but contains a large number of Asymptotic Giant Branch (AGB) and Red Giant Branch (RGB) stars). The disk of the galaxy is mostly dominated by red giant stars while its bulge consists of both the AGB and RGB population. Using the distance indicator technique, based on the tip of the red giant branch (TRGB), we find a distance of 3.42 ± 0.25 Mpc for this galaxy. Global photometric characteristic of this galaxy were then measured out to a radius of 3, giving V = 10m. 04 and I = 8m. 95. We find (V − I) = 0.3 for the nucleus of NGC 404. The integral colour of the galaxy changes slightly along the radius, and its mean value is (V − I) = 1.1. On the HST images situated at 9 from the galaxy center there are many red giants.
  • Announcement the President's Corner by Dell Vance, CVAS

    Announcement the President's Corner by Dell Vance, CVAS

    CVAS Executive Committee Pres – Dell Vance - (435) 938-8328 Loaner Scope Coordinator/NSN Coordinator – [email protected] Garrett Smith – [email protected] Vice Pres- Layne Pedersen – (801) 463-1701 Past President, Webmaster, Librarian – [email protected] Tom Westre – (435) 787-6380 [email protected] Treasurer- Brad Kropp - (435) 755-0877 Public Relations – Lyle Johnson - [email protected] [email protected] Secretary – Dale Hooper - (435) 563-0608 [email protected] Vol. 5 Number 3 November 2017 www.cvas-utahskies.org Meeting Announcement The President’s Corner By Dell Vance, CVAS President Our November meeting will be held on the third Wednesday in November, November 15, 2017 at 7pm in room 806/808 of the main BATC campus. Enter on the east side of the building located at 1301 North 600 West. Our featured speaker will be CVAS member Lyle Johnson. He will be speaking to us about “Backyard Astronomy for Beginners”. We will learn how to do backyard astronomy using only a free sky map, how to observe with ordinary binoculars and how to choose and use a telescope. This will be great information to help increase your enjoyment of the hobby. It will also be helpful if you or someone on your Christmas list is looking for binoculars or a telescope. Announcement I always love October. It is always a very busy month for me. That is a good thing. My wife and I The Executive Committee is interested in hearing usually go for drives and hikes through the canyons from the membership concerning meeting dates for with the fall colors.
  • Appendix II. Publications

    Appendix II. Publications

    Appendix II. Publications Gemini Staff Publications Papers in Peer-Reviewed Journals: Trujillo, Chadwick A.[2]. Detection of a Trailing (L5) Neptune Trojan. Science, 329:1304-. September, 2010. Leggett, S. K.[2]. A Detailed Model Atmosphere Analysis of Cool White Dwarfs in the Sloan Digital Sky Survey. The Astrophysical Journal Supplement, 190:77-99. September, 2010. Schiavon, Ricardo P.[3]. Dissecting the Red Sequence. IV. The Role of Truncation in the Two- dimensional Family of Early-type Galaxy Star Formation Histories. The Astrophysical Journal, 721:278-296. September, 2010. Hayward, Thomas L.[7]; Hartung, Markus[12]. The Gemini NICI Planet-finding Campaign: Discovery of a Close Substellar Companion to the Young Debris Disk Star PZ Tel. The Astrophysical Journal Letters, 720:L82-L87. September, 2010. Leggett, S. K.[1]. Properties of the T8.5 Dwarf Wolf 940 B. The Astrophysical Journal, 720:252- 258. September, 2010. McDermid, R. M.[16]. Formation of slowly rotating early-type galaxies via major mergers: a resolution study. Monthly Notices of the Royal Astronomical Society, 406:2405-2420. August, 2010. Leggett, S. K.[4]. 47 new T dwarfs from the UKIDSS Large Area Survey. Monthly Notices of the Royal Astronomical Society, 406:1885-1906. August, 2010. Hartung, M.[3]. Observations of a stationary mid-latitude cloud system on Titan. Icarus, 208:868- 877. August, 2010. Geballe, T. R.[2]. High-resolution 3-μm spectra of Jupiter: Latitudinal spectral variations influenced by molecules, clouds, and haze. Icarus, 208:837-849. August, 2010. McDermid, Richard M.[3]; Miller, Bryan W.[5]. The Einstein Cross: Constraint on Dark Matter from Stellar Dynamics and Gravitational Lensing.
  • Andromeda a Monthly Beginners Guide to the Night Sky by Tom Trusock

    Andromeda a Monthly Beginners Guide to the Night Sky by Tom Trusock

    CloudyNights Presents - Small Wonders: Andromeda A Monthly Beginners Guide to the Night Sky by Tom Trusock A printable version can be found here. Widefield Chart Target Name Type Size Mag RA DEC List beta Star 2.1 01h 09m 59.9s +35° 38' 41" gamma Star 2.1 02h 04m 11.9s +42° 21' 08" M 31 Galaxy 189.1'x61.7' 3.5 00h 43m 00.0s +41° 17' 36" M 32 Galaxy 8.5'x6.5' 8.1 00h 42m 57.5s +40° 53' 26" M 110 Galaxy 19.5'x11.5' 7.9 00h 40m 37.8s +41° 42' 36" NGC 404 Galaxy 3.5'x3.5' 10.0 01h 09m 42.8s +35° 44' 33" NGC 752 Open Cluster 75.0' 5.7 01h 57m 51.7s +37° 51' 19" NGC 7662 Planetary Nebula 37" 8.3 23h 26m 08.1s +42° 33' 38" Challenge Name Type Size Mag RA DEC Object NGC 891 Galaxy 11.7'x1.6' 10.1 02h 22m 50.5s +42° 22' 02" G1/Mayall II Globular Cluster 10" 13.7 00h 33m 02.6s +39° 36' 16" Andromeda, the daughter of Cassiopeia and Cepheus, was condemned to be sacrificed to Poseidon and bound to a rock near the shore. Just having returned after slaying the Gorgon, Perseus found, freed and married her. Andromeda is the 19th largest constellation in the night sky, now joins her mother, father, husband and his winged horse (Pegasus) in a seasonal procession around the pole. Far from resembling a Princess, I've always seen Andromeda as a cornucopia arriving just in time for harvest - whichever way you see it, it contains a wealth of spectacular deep sky objects.
  • Mirach's Goblin

    A&A 620, A126 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833302 & c ESO 2018 Astrophysics Mirach’s Goblin: Discovery of a dwarf spheroidal galaxy behind the Andromeda galaxy David Martínez-Delgado1, Eva K. Grebel1, Behnam Javanmardi2, Walter Boschin3,4,5 , Nicolas Longeard6, Julio A. Carballo-Bello7, Dmitry Makarov8, Michael A. Beasley4,5, Giuseppe Donatiello9, Martha P. Haynes10, Duncan A. Forbes11, and Aaron J. Romanowsky12,13 1 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany e-mail: [email protected] 2 School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran 19395-5531, Iran 3 Fundación G. Galilei – INAF (Telescopio Nazionale Galileo), Rambla J. A. Fernández Pérez 7, 38712 Breña Baja, La Palma, Spain 4 Instituto de Astrofísica de Canarias (IAC), Calle Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain 5 Departamento de Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain 6 Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, 67000 Strasbourg, France 7 Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, 782-0436 Macul, Santiago, Chile 8 Special Astrophysical Observatory, Nizhniy Arkhyz, Karachai-Cherkessia 369167, Russia 9 Nuovo Orione, 72024 Oria, Italy 10 Cornell Center for Astrophysics and Planetary Science, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA 11 Centre for Astrophysics & Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia 12 Department of Physics & Astronomy, San José State University, One Washington Square, San Jose, CA 95192, USA 13 University of California Observatories, 1156 High Street, Santa Cruz, CA 95064, USA Received 25 April 2018 / Accepted 9 October 2018 ABSTRACT Context.
  • The Ngc 404 Nucleus: Star Cluster and Possible Intermediate-Mass Black Hole

    The Ngc 404 Nucleus: Star Cluster and Possible Intermediate-Mass Black Hole

    The Astrophysical Journal, 714:713–731, 2010 May 1 doi:10.1088/0004-637X/714/1/713 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE NGC 404 NUCLEUS: STAR CLUSTER AND POSSIBLE INTERMEDIATE-MASS BLACK HOLE Anil C. Seth1,9, Michele Cappellari2, Nadine Neumayer3, Nelson Caldwell1, Nate Bastian4, Knut Olsen5, Robert D. Blum5, Victor P. Debattista6, Richard McDermid7, Thomas Puzia8, and Andrew Stephens7 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street Cambridge, MA 02138, USA; [email protected] 2 Sub-department of Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK 3 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 5 National Optical Astronomy Observatory, 950 North Cherry Ave., Tucson, AZ 85719, USA 6 Jeremiah Horrocks Institute, University of Central Lancashire, Preston, Lancashire, PR1 2HE, UK 7 Gemini Observatory, 670 N. A’ohoku Place Hilo, HI 96720, USA 8 Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada Received 2010 January 27; accepted 2010 March 1; published 2010 April 14 ABSTRACT We examine the nuclear morphology, kinematics, and stellar populations in nearby S0 galaxy NGC 404 using a combination of adaptive optics assisted near-IR integral-field spectroscopy, optical spectroscopy, and Hubble Space Telescope imaging. These observations enable study of the NGC 404 nucleus at a level of detail possible only in the nearest galaxies. The surface brightness profile suggests the presence of three components: a bulge, a nuclear star cluster (NSC), and a central light excess within the cluster at radii < 3 pc.