Palomar 14
{{ Infobox globular cluster
| name = Palomar 14
| image =
| epoch = J2000
| class =
| constellation = Hercules
| ra = {{RA|16|10|59.00}}{{cite simbad | title=GCl 38 | accessdate=2009-07-08}}
| dist_ly = {{nowrap|244,000 ly}}
| dist_pc = {{nowrap|74.7 kpc}}
| size_v =
| mass_kg =
| mass_msol =
| radius_ly =
| age = {{nowrap|10 Ga}}{{cite journal
| first=Michael | last=Hilker | date=March 11, 2006
| title=Probable Member Stars of the Gravitational Theory-Testing Globular Clusters AM 1, Pal 3 and Pal 14
| journal=Astronomy and Astrophysics | volume=448 | issue=1
| pages=171–180 | doi=10.1051/0004-6361:20054327 | bibcode=2006A&A...448..171H|arxiv = astro-ph/0510679 }}
| absmag_v =
| notes =
| names = GCl 38, Arp 1, {{nowrap|C1608 + 150}}
}}
Palomar 14 is a globular cluster located in the constellation Hercules. It is a member of the Palomar Globular Clusters group. Palomar 14 was discovered in 1958 by Sidney van den Bergh and Halton Arp during inspection of the photographic plates from the Palomar Sky Survey.{{cite journal
|author1=Arp, Halton |author2=van den Bergh, Sidney | date=1960
| title=A New Faint Globular Cluster
| journal=Publications of the Astronomical Society of the Pacific | volume=72 | issue=48 | pages=48
| doi=10.1086/127473 | bibcode=1960PASP...72...48A | doi-access=free }}
This is a round, diffuse cluster located in the outer
halo of the Milky Way galaxy. It is about 3–4 billion years younger than a typical galactic cluster.
The metallicity of the cluster is [Fe/H] = −1.50, indicating a lower abundance of elements with mass greater than helium compared to the Sun. The combined mass of the main sequence stars in the cluster is {{nowrap|1340 ± 50 solar masses}}, and the combined mass of observed stars within the half-light radius is {{nowrap|6020 ± 50 solar masses}}. (This is the inner radius of the cluster that emits half the total luminosity.) These mass estimates provide lower bounds for determining the total mass of the cluster. The median radial velocity of stars within the cluster is {{nowrap|72.19 ± 0.18 km/s}}.{{cite journal
|author1=Jordi, K. |author2=Grebel, E. K. |author3=Hilker, M. |author4=Baumgardt, H. |author5=Frank, M. |author6=Kroupa, P. |author7=Haghi, H. |author8=CBtE, P. |author9=Djorgovski, S. G. | title=Testing Fundamental Physics with Distant Star Clusters: Analysis of Observational Data on Palomar 14
| journal=The Astronomical Journal | volume=137 | issue=6
| pages=4586–4596 | date=2009
| doi=10.1088/0004-6256/137/6/4586
| bibcode=2009AJ....137.4586J |arxiv = 0903.4448 }}
Because of the cluster's location on the outer fringes of the Milky Way, it was used as a test case for modified Newtonian dynamics (MOND). This is an alternative hypothesis to explain the galactic rotation problem.