Ir Clusters Research Articles

Prototype Supported Metal Cluster Catalysts: Ir4 and Ir6

AbstractThe following is a review of the synthesis, chemistry, and catalytic properties of small, well‐defined supported metal clusters, Ir4 and Ir6. These supported clusters are synthesized either by adsorption of ligated molecular iridium clusters with tetrahedral and octahedral frameworks, for Ir4 and Ir6, respectively, or by adsorption of single‐iridium‐atom complexes followed by treatment to form clusters on the supports. The most insightful characterizations of supported metal clusters have been carried out by infrared and X‐ray absorption spectroscopies and aberration‐corrected scanning transmission electron microscopy. Reactions of the supported clusters include ligand modifications and ligand removal, oxidative fragmentation, and migration leading to metal aggregation. Reactivities and catalytic properties of the clusters (e.g., for olefin hydrogenation) depend on the cluster size and the support (which acts as a ligand) and are distinct from those of supported particles that resemble bulk iridium. Transient spectroscopic data illustrate that the structures of the active species in ethylene hydrogenation catalysis switch reversibly from Ir4 to single‐iridium‐atom complexes in response to changes in the ethylene/H2 ratio in the gas phase. Density functional theory has been used to predict properties of these clusters, notably their ability to add hydrogen, and the agreement between theory and experiment is good. Recent advances in the characterization of supported Ir4 and Ir6 clusters have been crucial in the elucidation of their behavior, and these methods apply as well to the more complicated structures of industrial supported metal catalysts.

A submillimetre survey of the kinematics of the Perseus molecular cloud - III. Clump kinematics

We explore the kinematics of continuum clumps in the Perseus molecular cloud, derived from C18O J=3-2 data. Two populations are examined, identified using the automated algorithms CLFIND and GAUSSCLUMPS on existing SCUBA data. The clumps have supersonic linewidths with distributions which suggest the C18O line probes a lower-density 'envelope' rather than a dense inner core. Similar linewidth distributions for protostellar and starless clumps implies protostars do not have a significant impact on their immediate environment. The proximity to an active young stellar cluster seems to affect the linewidths: those in NGC1333 are greater than elsewhere. In IC348 the proximity to the old IR cluster has little influence, with the linewidths being the smallest of all. A virial analysis suggests that the clumps are bound and close to equipartition. In particular, the starless clumps occupy the same parameter space as the protostars, suggesting they are true stellar precursors and will go on to form stars. We also search for ordered C18O velocity gradients across the face of each core, usually interpreted as rotation. We note a correlation between the directions of the identified gradients and outflows across protostars, indicating we may not have a purely rotational signature. The fitted gradients are larger than found in previous work, probably as a result of the higher resolution of our data and/or outflow contamination. These gradients, if interpreted solely in terms of rotation, suggest that rotation is not dynamically significant. Furthermore, derived specific angular momenta are smaller than observed in previous studies, centred around j~0.001 km/s pc, which indicates we have identified lower levels of rotation, or that the C18O J=3-2 line probes conditions significantly denser and/or colder than n~10^5 per cc and T~10 K.

Theoretical study of ethene hydrogenation reaction on Ir4 tetrahedral cluster

AbstractHydrogenation reaction of ethene on free Ir4 cluster was theoretically investigated using DFT B3LYP level of theory with LanL2Dz basis set. It was found that hydrogen molecule adsorption proceeded without an apparent transition state structure and the adsorption energy was predicted to be −93.7 kJ/mol. Two possible channel of hydrogenation reaction were investigated. Distortion of cluster frame and high values of activation energies make these channels unfavorable. It was shown that inclusion of magnesium oxide (MgO) support model in our calculations account for a considerable variation of geometric parameters of Ir4 cluster. The bonding of a single carbon ligand to the supported tetrahedral Ir4 cluster at the on‐top site was also modeled to probe changes in geometric parameters in comparison with unsupported cluster. © 2010 Wiley Periodicals, Inc. Int J Quantum Chem, 2011

Role of Adsorbed H, C, O, and CO on the Atomic Structure of Free and MgO(100)-Supported Ir4Clusters: An ab Initio Study

We applied density functional theory based on ultrasoft pseudopotentials to study the structural properties of Ir4 clusters both in the gas phase and adsorbed on a MgO(100) surface. To resolve the discrepancy between experimental data which suggest a tetrahedral structure for Ir4 and theoretical results which show a strong preference for the square isomer, we investigated the effect of several adsorbates on the equilibrium atomic structure of the clusters. Calculated binding energies of a single H, C, or O atom, as well as one CO or OH molecule, to three stable Ir4 isomers indicate that C or CO adsorption significantly influences the relative stability of Ir4 isomers. For MgO(100)-supported Ir4, atomic carbon is able to change the isomer preference from the square to the tetrahedral geometry.

Mercaptosilane-Assisted Synthesis of Metal Clusters within Zeolites and Catalytic Consequences of Encapsulation

We report here a general synthetic strategy to encapsulate metal clusters within zeolites during their hydrothermal crystallization. Precursors to metal clusters are stabilized against their premature colloidal precipitation as hydroxides during zeolite crystallization using bifunctional (3-mercaptopropyl)trimethoxysilane ligands. Mercapto (-SH) groups in these ligands interact with cationic metal centers, while alkoxysilane moieties form covalent Si-O-Si or Si-O-Al linkages that promote zeolite nucleation around ligated metal precursors. These protocols led to the successful encapsulation of Pt, Pd, Ir, Rh, and Ag clusters within the NaA zeolite, for which small channel apertures (0.41 nm) preclude postsynthesis deposition of metal clusters. Sequential treatments in O(2) and H(2) formed small (approximately 1 nm) clusters with uniform diameter. Titration of exposed atoms with H(2) or O(2) gave metal dispersions that agree well with mean cluster sizes measured from electron microscopy and X-ray absorption spectroscopy, consistent with accessible cluster surfaces free of mercaptosilane residues. NaA micropore apertures restrict access to encapsulated clusters by reactants based on their molecular size. The ratio of the rates of hydrogenation of ethene and isobutene is much higher on clusters encapsulated within NaA than those dispersed on SiO(2), as also found for the relative rates of methanol and isobutanol oxidation. These data confirm the high encapsulation selectivity achieved by these synthetic protocols and the ability of NaA micropores to sieve reactants based on molecular size. Containment within small micropores also protects clusters against thermal sintering and prevents poisoning of active sites by organosulfur species, thus allowing alkene hydrogenation to persist even in the presence of thiophene. The bifunctional nature and remarkable specificity of the mercapto and alkoxysilane functions for metal and zeolite precursors, respectively, render these protocols extendable to diverse metal-zeolite systems useful as shape-selective catalysts in demanding chemical environments.

ChemInform Abstract: Supported Metal Cluster Catalysts

Abstract Highly dispersed metal catalysts containing supported clusters of only several metal atoms each, exemplified by Ir 4 and Ir 6 , were prepared by removal of CO ligands from supported precursors, for example, [Ir 4 (CO) 12 ] and [Ir 6 (CO) 16 ]. Transmission electron microscopy (TEM), extended X-ray absorption fine structure spectroscopy and density functional theory indicate the metal–support-oxygen coordination numbers and distances, which identify the supports as multidentate oxygen-donor ligands. Theory indicates that Ir 4 clusters in zeolite NaX are neutral or slightly negatively charged and that cluster-support bonding induces a polarization of the cluster that could affect reactivity and catalysis. Supported catalysts prepared from precursors with noble metal-oxophilic metal bonds are modeled as clusters of a few atoms of the noble metal ‘nested’ in a supported cluster of the oxophilic metal oxide, which helps to anchor and stabilize the noble metal clusters. Changes in the oxide support have only modest effects on the catalytic activities of supported metal clusters for toluene hydrogenation, but the catalytic activity of γ-Al 2 O 3 -supported Ir clusters per exposed Ir atom increases with increasing cluster size, and this observation remains to be explained.

Operando study of iridium acetylacetonate decomposition on amorphous silica–alumina for bifunctional catalyst preparation

The decomposition of iridium acetylacetonate Ir(acac)(3) impregnated on amorphous silica-alumina (ASA) has been investigated by combined thermogravimetry-differential thermal analysis-mass spectrometry (TG-DTA-MS) and by in situ X-ray diffraction (XRD). The resulting Ir/ASA hydrotreating catalysts have also been characterized by transmission electron microscopy (TEM). The effects of heating treatments under oxidative, reductive or inert gas flows are compared with each other and with similar experiments on ASA-supported acetylacetone (acacH). It is shown that Ir(acac)(3) undergoes exothermic combustion during calcination in air, leading to agglomerated IrO(2) particles. Conversely, direct reduction involves hydrogenolysis of the acac followed by hydrogenation of the ligand residues to alkanes and water. These two processes are catalyzed by Ir clusters, the gradual growth of which is followed in situ by XRD. The resulting nanoparticles are highly and homogeneously dispersed.

Discovery of large-scale gravitational infall in a massive protostellar cluster

We report Mopra (ATNF), Anglo-Australian Telescope, and Atacama Submillimeter Telescope Experiment observations of a molecular clump in Carina, BYF73 = G286.21+0.17, which give evidence of large-scale gravitational infall in the dense gas. From the millimetre and far-infrared data, the clump has mass ~ 2 x 10^4 Msun, luminosity ~ 2-3 x 10^4 Lsun, and diameter ~ 0.9 pc. From radiative transfer modelling, we derive a mass infall rate ~ 3.4 x 10^-2 Msun yr-1. If confirmed, this rate for gravitational infall in a molecular core or clump may be the highest yet seen. The near-infrared K-band imaging shows an adjacent compact HII region and IR cluster surrounded by a shell-like photodissociation region showing H2 emission. At the molecular infall peak, the K imaging also reveals a deeply embedded group of stars with associated H2 emission. The combination of these features is very unusual and we suggest they indicate the ongoing formation of a massive star cluster. We discuss the implications of these data for competing theories of massive star formation.

A versatile fabrication method for cluster superlattices

On the graphene moiré on Ir(111) a variety of highly perfect cluster superlattices can be grown as shown for Ir, Pt, W and Re. Even materials that do not form cluster superlattices upon room temperature deposition may be grown into such by low-temperature deposition or the application of cluster seeding through Ir as shown for Au, AuIr and FeIr. Criteria for the suitability of a material to form a superlattice are given and largely confirmed. It is proven that at least Pt and Ir form epitaxial cluster superlattices. The temperature stability of the cluster superlattices is investigated and understood on the basis of positional fluctuations of the clusters around their sites of minimum potential energy. The binding sites of Ir, Pt, W and Re cluster superlattices are determined and the ability to cover samples macroscopically with a variety of superlattices is demonstrated.

Cluster size effects on sintering, CO adsorption, and implantation in Ir/SiO2

A series of planar model catalysts have been prepared via deposition of Ir(n) (+) on thermally grown amorphous SiO(2)/Si(100) and ion scattering spectroscopy was used to probe surface structure as a function of cluster size, impact energy, and surface temperature. Deposition of Ir(2) or Ir(10) at low energies and room temperature results in stable clusters forming one- or two-dimensional single layer islands on the oxide surface. Heating the samples to 750 K leads to agglomeration, forming multilayer structures on the surface. Ir(1) deposited under similar conditions sinters into large clusters at room temperature. Deposition at 110 K at least partially stabilizes the Ir atoms with respect to diffusion and sintering. At higher deposition energies, partial implantation into the surface is observed, but this appears to be insufficient to stabilize the clusters against sintering at elevated temperature. At low temperatures, substrate-mediated adsorption of CO is found to be highly efficient, leading to near saturation coverages of CO bound atop the Ir(n) clusters. The CO can be removed by careful He(+) sputtering. The deposition/binding behavior of Ir(n) on SiO(2) is quite different from Ir(n)/TiO(2)(110), for which the clusters bind in three-dimensional morphology, starting at Ir(5). That system also shows substrate-mediated adsorption of CO, but the CO preferentially binds at the periphery of the clusters rather than on top.

PAMAM Dendrimer-Derived Ir/Al2O3 Catalysts: An EXAFS Characterization

Extended X-ray absorption fine structure (EXAFS) spectroscopy was used to characterize several synthesis stages of hydroxyl-terminated generation four (G4OH) PAMAM dendrimer-derived Ir/γ-Al2O3 catalyst. The EXAFS results indicate that Ir3+ forms complexes with dendrimer functional groups through displacement of two Cl− ion ligands. These complexes are very stable in solution, and no reduction of Ir3+ to Ir nanoparticles or clusters is observed after introduction of reducing agents such as NaBH4 or H2. These Ir3+-dendrimer complexes remain essentially intact after support impregnation. The formation of 1–2 nm particles occurs when the catalysts are treated with O2/H2 or H2, and the dendrimer-derived catalysts exhibit a lower degree of metal support interaction.

CHANDRAANDSPITZERIMAGING OF THE INFRARED CLUSTER IN NGC 2071

We present results of a sensitive Chandra X-ray observation and Spitzer mid-infrared (mid-IR) observations of the IR cluster lying north of the NGC 2071 reflection nebula in the Orion B molecular cloud. We focus on the dense cluster core known as NGC 2071-IR, which contains at least nine IR sources within a 40'' x 40'' region. This region shows clear signs of active star formation including powerful molecular outflows, Herbig-Haro objects, and both OH and H{sub 2}O masers. We use Spitzer Infrared Array Camera (IRAC) images to aid in X-ray source identification and to determine young stellar object (YSO) classes using mid-IR colors. Spitzer IRAC colors show that the luminous source IRS 1 is a class I protostar. IRS 1 is believed to be driving a powerful bipolar molecular outflow and may be an embedded B-type star or its progenitor. Its X-ray spectrum reveals a fluorescent Fe emission line at 6.4 keV, arising in cold material near the protostar. The line is present even in the absence of large flares, raising questions about the nature of the ionizing mechanism responsible for producing the 6.4 keV fluorescent line. Chandra also detects X-ray sources at or near the positions of IRS 2,more » IRS 3, IRS 4, and IRS 6 and a variable X-ray source coincident with the radio source VLA 1, located just 2'' north of IRS 1. No IR data are yet available to determine a YSO classification for VLA 1, but its high X-ray absorption shows that it is even more deeply embedded than IRS 1, suggesting that it could be an even younger, less-evolved protostar.« less

ACHANDRASTUDY OF THE ROSETTE STAR-FORMING COMPLEX. II. CLUSTERS IN THE ROSETTE MOLECULAR CLOUD

We explore here the young stellar populations in the Rosette Molecular Cloud (RMC) region with high spatial resolution X-ray images from the Chandra X-ray Observatory, which are effective in locating weak-lined T Tauri stars as well as disk-bearing young stars. A total of 395 X-ray point sources are detected, 299 of which (76%) have an optical or near-infrared (NIR) counterpart identified from deep FLAMINGOS images. From X-ray and mass sensitivity limits, we infer a total population of about 1700 young stars in the survey region. Based on smoothed stellar surface density maps, we investigate the spatial distribution of the X-ray sources and define three distinctive structures and substructures within them. Structures B and C are associated with previously known embedded IR clusters, while structure A is a new X-ray-identified unobscured cluster. A high mass protostar RMCX #89 = IRAS 06306+0437 and its associated sparse cluster is studied. The different subregions are not coeval but do not show a simple spatial-age pattern. Disk fractions vary between subregions and are generally 20% of the total stellar population inferred from the X-ray survey. The data are consistent with speculations that triggered star formation around the HII region is present in the RMC, but do not support a simple sequential triggering process through the cloud interior. While a significant fraction of young stars are located in a distributed population throughout the RMC region, it is not clear they originated in clustered environments.

THE INTERMEDIATE-MASS EMBEDDED CLUSTER GM 24 REVISITED: NEW INFRARED AND RADIO OBSERVATIONS

New and archived high-resolution infrared (IR; 1–20 μm) and radio-continuum images of the isolated embedded cluster and associated compact H ii region, GM 24, are presented and measured photometrically. The nucleus of the complex is Irs 3, or IRAS 17136-3617, located at the densest part of the molecular cloud. This object is composed of at least three compact near-IR sources (A, B, and C) that are the most luminous and massive young stellar components and provide most of the ionizing energy to the cometary-shaped radio H ii region. The 3.6 cm radio map shows a complex structure with an extended emission peak and two very compact components very close to Irs 3A. Large inhomogeneities in the dust density within the nebula cause considerably different morphologies in the observed emission of hydrogen recombination lines, namely Paβ, Brγ, and Brα. No H2 line emission at 2.12 μm was detected. The embedded IR cluster is found to contain more than 100 members within a radius of around 40'', which corresponds to 0.39 pc. The total stellar mass is estimated to be ⩾250 M☉. The extinction to the nearby edge of the cluster is determined to be AV = 13, though a number of sources, including Irs 3, are reddened by AV > 50. A fraction of near-IR sources, mainly in the periphery of the cluster, are main-sequence A–B-type stars, while a large fraction (∼50%) of the detected members show significant IR excesses, including several Class I young stellar objects with luminosities ranging from a few solar luminosities near our sensitivity limit, to 1.5 × 105 L☉, the derived luminosity of Irs 3.

Synthesis and characterization of heterometallic M–Ru (M = Co, Rh, Ir) clusters containing the nido-dicarborane-1,2-dithiolato chelating ligand

The 16-electron half-sandwich complexes Cp*M[S(2)C(2)(B(10)H(10))] (M = Ir (1), Rh (2), Co (3)) react with [Ru(COD)Cl(2)](x) under basic conditions at 35-40 degrees C to give different hetero-dinuclear clusters {Cp*M[S(2)C(2)(B(9)H(10))]}Ru(COD) (M = Ir (1a), Rh (2a), Co (3a)) and {Cp*M[S(2)C(2)(B(9)H(9))]}Ru(COD)(OCH(3)) (M = Ir (1b), Rh (2b), Co (3b)) with open carborane cages. Moreover, B-H-->Ru bridge bonds were observed in complexes 1a, 2a,3a . In reaction a, minor products trinuclear complex {Cp*Ir[S(2)C(2)(B(10)H(10))]}(2)Ru (1c) and methoxyl-disubstituted complex Cp*Ir[S(2)C(2)(B(10)H(8))(OCH(3))(2)] (1d) were successfully isolated. However, when the reaction temperature decreased to 0-10 degrees C, the kinetically-controlled products, mono-substituted complex Cp*Ir[S(2)C(2)(B(10)H(9))(OCH(3))] (1e) and disubstituted complex Cp*Ir[S(2)C(2)(B(10)H(8))(OCH(3))(2)] (1d), were isolated as the main products; nevertheless, the thermodynamically-controlled products, open-carborane complexes 1a and 1b , were isolated as the minor products. In complex Cp*Co[S(2)C(2)(B(9)H(10))]Ru(C(7)H(8)) (3c), one COD coordinated to ruthenium has been replaced by toluene. The reactions demonstrate that different types of products can be obtained by controlling the reaction conditions. All these new complexes have been characterized by IR, (1)H NMR, (11)B NMR and elemental analyses. The molecular structures of 1a, 1b, 1c, 1d, 1e, 2a and 3a have also been determined by single-crystal X-ray diffraction analyses.

Hydrogen Adsorption on Zeolite-Supported Tetrairidium Clusters. Thermodynamic Modeling from Density Functional Calculations

Using energetic and spectral data from density functional calculations on a series of model species, hydrogenated clusters Ir4Hn with up to n = 12 H atoms on a dehydroxylated zeolite support, we established a thermodynamic model of hydrogen loading on zeolite-supported Ir4 clusters that accounts for temperature and H2 pressure. The average number of H ligands, <n>, on the metal moiety was determined as function of temperature and H2 pressure. These results indicate that species with different hydrogen loading should be observable. Thus, the actual hydrogen loading of supported Ir4 clusters is predicted to depend strongly on the pretreatment and the conditions at which the system is examined. The reported thermodynamic data should be helpful for controlling the hydrogen loading of such clusters via temperature and H2 pressure. They also permit one to determine conditions for the total dehydrogenation of the clusters or for preparing species with particularly high hydrogen loading. The latter is especially important for hydrogenation/dehydrogenation processes over supported metal catalysts.

Fe–Rh and Fe–Ir clusters substituted by diphenylacetylene: Synthesis, solid state structure and electrochemical behaviour of [Fe 2Ir 2(CO) 10(μ 4:η 2-PhCCPh)] 2−, [FeIr 2(CO) 9(μ 3:η 2-PhCCPh)], and [Fe 2Rh(CO) 8(μ 3:η 2-PhCCPh)] −

The reaction between [Fe 2Ir 2(CO) 12] 2− and diphenylacetylene in refluxing CH 3CN yields the substituted cluster [Fe 2Ir 2(CO) 10(PhC 2Ph)] 2− ( 1). In the crystals, the four metal atoms define a butterfly arrangement whose Ir–Ir hinge is parallel to the acetylenic C 2 unit. The neutral triangular cluster [FeIr 2(CO) 9(PhC 2Ph)] ( 2) is obtained by the treatment of 1 with acids at room temperature; in this 48 valence electrons species, the C–C and the Ir–Ir bonds are also parallel, in the μ 3 – η ∥ 2 coordination mode. The cluster [Fe 2Rh(CO) 10] − reacts with diphenylacetylene in refluxing THF yielding [Fe 2Rh(CO) 8(PhC 2Ph)] − ( 3). In this 46 C.V.E.’s cluster, the C 2 unit is perpendicular to the Fe–Fe edge, exemplifying the μ 3 – η ⊥ 2 bonding mode. According to 13C NMR spectra, the structure of the three clusters is maintained in solution. Electrochemical investigations show that the one-electron oxidation of [Fe 2Ir 2(CO) 10(L)] 2− (L = 2CO, PhC 2Ph) as well as the one-electron reduction of [Fe 2Rh(CO) 8(PhC 2Ph)] − only generates the respective short lived products.

Investigation of the conspicuous infrared star cluster and star-forming region “RCW 38 IR Cluster”

The infrared star cluster RCW 38 IR Cluster, which is also a massive star-forming region, is investigated. The results of observations with the SEST (Cerro La Silla, Chile) telescope on the 2.6-mm 12CO spectral line and with SIMBA on the 1.2-mm continuum are given. The 12CO observations revealed the existence of several molecular clouds, two of which (clouds 1 and 2) are connected with the object RCW 38 IR Cluster. Cloud 1 is a massive cloud, which has a depression in which the investigated object is embedded. It is not excluded that the depression was formed by the wind and/or emission from the young bright stars belonging to the star cluster. Rotation of cloud 2, around the axis having SE-NW direction, with an angular velocity ω = 4.6 · 10−14 s−1 is also found. A red-shifted outflow with velocity ∼+5.6 km/s, in the SE direction and perpendicular to the elongation of cloud 2 has also been found. The investigated cluster is associated with an IR point source IRAS 08573-4718, which has IR colors typical for a non-evolved embedded (in the cloud) stellar object. The cluster is also connected with a water maser. The SIMBA image shows the existence of a central bright condensation, coinciding with the cluster itself, and two extensions. One of these extensions (the one with SW-NE direction) coincides, both in place and shape, with cloud 2, so that the possibility that this extension might also be rotating like cloud 2 is not excluded. In the vicinity of these extensions there are condensations resembling HH objects.

Density Functional Study of Hydrogen Adsorption on Tetrairidium Supported on Hydroxylated and Dehydroxylated Zeolite Surfaces

We explored computationally successive adsorption of hydrogen on Ir4 clusters both in the gas phase and on hydroxylated or dehydroxylated zeolite support, the latter described by cluster models. Free and supported Ir4 clusters studied were calculated to adsorb dissociatively large amounts of hydrogen, up to three hydrogen atoms per metal atom. In the range covered, the energy for dissociative adsorption of hydrogen on Ir4Hx clusters (x = 0, 3, 6, 9, 12) in the gas phase is almost independent of x, ∼70 kJ/mol per adsorbed atom. The corresponding energy gain is smaller for zeolite-supported Ir4. The average Ir−Ir distance of free and supported clusters increases with hydrogen loading at very similar rates, by ∼1.9 pm per adsorbate. Charged Ir4Hx complexes adsorbed on a dehydroxylated zeolite surface are always more stable than complexes of the same chemical composition in gas phase or supported on a hydroxylated surface. Therefore, reverse hydrogen spillover from OH groups of the support onto the metal cluster is calculated to be energetically favorable not only for bare clusters but also after partial loading of hydrogen. From the calculated structural and energetic parameters we suggest that the tetrairidium species in faujasite-type zeolites, produced experimentally and investigated by extended X-ray absorption fine structure (EXAFS), correspond to hydrogenated moieties Ir4Hx (x = 9−12) supported on a dehydroxylated framework.

IR Observations of MS 1054−03: Star Formation and Its Evolution in Rich Galaxy Clusters

We study the IR properties of galaxies in the cluster MS 1054-03 at z = 0.83 by combining MIPS 24 μm data with spectra of more than 400 galaxies and a very deep K-band-selected catalog. Nineteen IR cluster members are selected spectroscopically, and an additional 15 are selected by their photometric redshifts. We derive the IR luminosity function of the cluster and find strong evolution compared to the similar-mass Coma Cluster. The best-fitting Schechter function gives L = 11.49 L☉ with a fixed faint-end slope, about 1 order of magnitude larger than that in Coma. The rate of evolution of the IR luminosity from Coma to MS 1054-03 is consistent with that found in field galaxies, and it suggests that some internal mechanism, e.g., the consumption of the gas fuel, is responsible for the general decline of the cosmic SFR in different environments. The mass-normalized integrated SFR within 0.5R200 in MS 1054-03 also shows evolution compared with other rich clusters at lower redshifts, but the trend is less conclusive if the mass selection effect is considered. A nonnegligible fraction (13% ± 3%) of cluster members are forming stars actively, and the overdensity of IR galaxies is about 20 compared to the field. It is unlikely that clusters only passively accrete star-forming galaxies from the surrounding fields and have their star formation quenched quickly afterward; instead, many cluster galaxies still have large amounts of gas, and their star formation may be enhanced by the interaction with the cluster.